(SANITIZED)UNCLASSIFIED SOVIET PAPERS ON SPACE RESEARCH(SANITIZED)

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP80T00246A016600420001-1
• Release Decision: RIPPUB
• Original Classification: C
• Document Page Count: 493
• Document Creation Date: December 22, 2016
• Document Release Date: December 8, 2011
• Sequence Number: 1
• Publication Date: May 24, 1962
• Content Type: REPORT

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A TO THi RESULTS OF TH CHAKGJ D YA.-t'1' LCLi THH! ~-
ELLCT PODE TRAr XPE1ZI;11TS LI THi SEC0UD RADIATION
liLbT AND IN THE 0U'1'E li;iOST 3. L'T OF CHARGED YARTICLL'S
j A.T.Grin au z, S.L.Balandiria, G.A. Bordovs1 y.
N.P.I.Shutte
Abstr act
Results are presented of the .laboratory experiments with
charged particle traps identical with those installed on
radiation belt.
In the papers
Soviet space probes. It
f icie:itly record fluxes
order of tens of keys.
T1e data presented
absence of considerable
is shown that the traps highly ef-
of electrons with energies on the
confirm the conclusion about the
soft electron fluxes in the outer
by S.1'.Verr;ov, A.E.Chudakov and others
(1), (2) and b;; J.A.Van Allen, J.A.Simpson, R.L.Arnoldy and
others (3)-(6) published in 1959-1961 and devoted to des-
criptions of the outer radi- tion belt investi,;;ations the
electron flux values determined by the authors were estima-
ted as 1010-1O11 crn 2sec-1. These estimates contradicted to
the results of measurements of the currents produced by the
fluxes of charged parL:icles gettin, into three-electrode
traps mounted on the a ame space probes as the instruments
used by S.N.Vernov and others (2). In the papers by
K.I.Gringauz, V.G.Kurt, V.I. 1,1oVDz and I.S.Shklovsky published
in April-July 1960 (7), (8), it as pointed out that the
upper boundary of electron fluxes in the outer radiation
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belt did nbt exceed (2-;3) 107cm -2 sec-1 during the experi-
ments (l)--(6). It was pointed out that the count4 rates
observed in experiments with cosmic ray counters (l)-(6)
should be accounted for not by the influence of soft elec-
trons with the maximum energy distribution lying in the re-
gion of -30 Kev, as it was done in (l)-(6), but by the ac-
t ion of electron fluxes which are not less than by 103
times lower than those given in the papers by J.Van Allen,
S.N.Vernov et al. and with much greater energies.
In Fig.l a diagram is presented of the spatial distri-
bution of the charged particle belts around the Earth from
the paper (7). On this figure there are also indicated the
estimates of the f luxes in the second belt and in the oute-,. -
most belt of charged particles which was discovered during
the same three-electrode trap experiments.
In the outermost belt which vas not detected by the cos-
mic ray counters the electron fluxes were recorded with
energies more than 200 ev and lower than -.-20 kev which
exceeded the electron fluxes in the secondtbelt by an order
of magnitude.
The authors of the present report subjected the traps
identical in their design to those used on Lunik II to the
irradiation by electron fluxes with energies which .were
ascribed to soft electrons in the second and outermost
belts. The aim of the experiment was. to get convinced that
the absence of considerable negative currents in the traps
during the space rockets passage through the second
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radiation belt is not due to some spurious effects (of the
type of the considerable secondary electron emission from
the collector under the action of soft electron fluxes. in the
radiation belt). At the same time it was necessary to esti-
mate errors in the determination of electron fluxes in the
outermost belt due to the same reasons. The results of these
experiments were mentioned in the report by K.I.Gringauz at
the Second International Space Science Symposium in Florence
in 1961 (9). At present we are going to give more detailed
data.
The diagram of the experiment is press ted in Fig.2.
The electron flux produced by, an electron gun (1) was
focussed by means of a cylinder (2). The voltage variation
on the cylinder with respect to the anode (3) has made it
possible to change the energy of electrons from 150 ev to
40 kev. Control measurements of the value of the total cur-
rent were carried out by means of a special probe (4) which
was put on the w ay of the stream and whose`design ensured the
possibility of conducting; absolute measurements. After each
control measurement the probe was removed. The degree of
the focussing of the electron beam was checked up by means
of a removable juminescent screen (5). The trap (6) could
be turned relative to the direction of the electron flux.
The voltages on its outer and inner grids could vary during
the experiment.
Fig.3 gives the dependencies of the current in the
circuit of the trap collector from the inner ;rid potential
at different energies of the electrons of the incident strean:
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and at its constant value (I,=5.10 9 amperes).
The upper scale of the abscissa shows the ca,
inner grid potential with respect to the zero level
which corresponds to the potential of the body of the instru-
mentation container. The lower scale shows the variation of
the inner grid potential fit C with respect to the collec-
tj . From the curves of Fig-3 one can see the well known
effect of the decrease of the secondary electron emission co-
ef f is ient with the increase of the energy of primary elec-
trons (10). The measured negative collector current also
decreases with the increase of the energy of the incident
stream. For each value of the energy of the incident stream
the 131 change in the interval from - 15U t o - 200 volts does
not cause any change in the collector current. The m llec-
tor current decrease is accounted for chiefly by the fact
that with the increase of the primary flux energy the por-
tion increases of electrons leaving the collector surface
with high velocity (inelastickally scattered or reflected
electrons) which co2respondingly cannot be retarded by the
inner grid =-200 volts) (11), (12).
Fig;.4 gives the depencencea of the ratio of the collec-
tor current IC , to the value of the curreniI0 , which cor-
responds to the inc ident electron flux measured 'by means of a
control probe, on the energy of the incident electron fluxes
different in the magnitude (I. varied from 10-1U amp. to
5-10-9 amp.) In the inner grid the constant potential
=-200 volts was kept, and the outer grid potential
,,,varied from 0 to + 50 volts. From the curves of Fig.4 is
evident that the IJIo ratio in the investigated energy
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range does not practically vary at considerable variations
of the incident electron current. Thus it is evident that
the values of the fluxes of electrons with elier ies up to
40 Kev determined by means of three-electrode traps of, the
type installed on Lunik II have turned to be not more than
by 2=3 tiraes lower than the actual values. From this it
f olloww,s that the estimate of the order of magnitude of elec-
tron currents with the above indicated ener,;ies by means of
such traps is correct.
It should ce noted that the recorded collector currents
o~' the traps of the type consider(id can be determined gen-
erally speeki:',.g by the difference of the electron fluxes
with energies exceedinge~a, is the negative potential of
the inner grid) and the fluxes of protons with energies more
than e~q~ C~qi is the positive potential of the outer grid).
However, the probability that at the registration of
the electron flux there is considerable compensation of the
electron current by the proton, one is small. if we assume
that he co~-,centratiori of energetic protons is equal to that
of energetic electrons, the energy of protons which would be
able to compensate for the current produced by electrons
should be by three orders of magnitude higher than the
energy of electrons. This meal that the fluxes of electrons
vaith energies of the order of tens of keys would be able to
be compensated by the f luxes of protons with energies of
the order of rnev As followa from (13), such protons at
the trap nickel collector 0.3 ram thick could b,, recorded
only with very love efficiency.
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 _ ... l.l. ll .... .w w _1..J it l i . ~_ _.
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Let us not', that co it iollov,s from (14) electrons with
.:e 1 s up to tc,:: oi c,(-,VS hold L':. _'etahded by suca la
co1Z.. c t c t'` iVely/~- k e ,ecol6L ~ i.e ; ~.
Thuss the experiments confirmed the cor"ec tress o--'. the
cone J_u i:r, drawn in (7) and (8) (1960) that in the second
_.e,distion belt the fluxes of soft electrons do not exceed
unities per 101cm-2 ::cc-1 and the sou. tip g: rote in Lhc
ch r 'ed o!irticle co:.nters observed in the second belt is not
ne to la~,~a fluxes of electrons with enemies of the order
of tens of la-,vs, but due to fluxes of much mor:: energetic
particles.
In conclusion we shall consider the renark by Winckler
and Kello(15) referring to the results of mencure.ilents
mod e by means of thy, traps in the outermost belt of charted
particles. According to calculations carried out by the
authors (15) the electron currents in the outermost belt
should be on the order of 109 el/cm2 sec.
The traps experimc--nt s (16) have given the value of the
flux equal to 2.108 el/cm2 sec. Winckler and Kello_;g have
pointed out that during the above mentioned measurements
the amplifiers of the traps were close to saturation and
would not be able to measure electron currents of the order
of 109 ,elicm2 sec which should have taken place according
to their calculations. This remark is correct. Une ':-zho ilc,
however, bear in mind that the measured currents quite
definitely have, not reached the amplifier satu:ciryti-n level.
On the other hand, since the traps could not record fluxes
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of electrons with energies lower than 200 ev,it is quite
probable that the total flux can reach 'the value of 109 el/cm-
see precisely due to the electrons with energies Et200 ev.
Electrons with energies of 10 kev recorded by L.R.Davis
(17) in the region of the outermost belt on the Explorer XII
satellite have apparently belonged to. the energetic portion
of the electron spectrum of this belt.
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 . .. . ...:. .._ll.-11 ...w ..-- ]JI ._.- ... ....1-- _ ....
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F.0 I RrNCES
1. 8.N.Vernov, A.E.Chudakov, ..V. Vakulov, Yu.I.1+o;achev,
Dokl.Akad.Nauk SSSR. 125, 304, 1959.
2. S.N.Vernov, A.E.Chudakov, r.V.Vakulov, YU.I.i,ogachev,
A.T.Nikolayev, Dokl.Akad. Nauk SSSR, 130, 517, 1960.
3. J.A.Van Allen, U.A.Frank, Nature, 183, 430, 1959.
4. J.A.Van Allen, u.A.Frank, Natut'e, 184, 919, 1959.
5. Ii.L.Arnoldy, R.A.Hoffman, J.R.Winckler, J.Geophys.Res.,65,
1361-1375, 1960.
6. C.J.Fan, P.I;iej r, J.A.Simpson, J.Geophys.Re4., 66, 26u7-
264U, 1961.
7. K.I.Grin,,.auz, V.G.Kurt, V.I.Moroz, I.S.Shklovsky, Dokl.
Akad.Nauk. SSSR, 132, 1062, 1960.
8. K.I.Gringauz, V.G.Kurt, V.I.Moroz, I.S.Shklovsky, Astronom.
Zhurnal, 34, 4, 19o0.
9. K.I.Gringauz, Space Research II edited by H.C. van de Hul;,.t
C. de Jager, A.F.Moor, 539, Amsterdam, 1961.
1/. Trump, van de Craaf, J. of Applied Physics, 18, 327, 1947.
11. H.I.assey and E.Burhop, Electronic and Ionic Impact Pheno-
mena, Russian translation, Mo; cow, 1958.
12. N.D.Mor;ulis, rroceedin,s of the Conference on the Catnode
Electronics, Kiev, 1951.
13. H.Smith, Physical Review, 71, 32, 1947.
14. L.Spencer, Physical Review, 98, 1597, 1955.
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15. P.J.Kello:_;g, J.R.Winckler, J.Geophys. Res.,66,12,1961.
16. K.I.Gringauz, V.V.Bezrukikh, V.D.Ozerov, R.E.Rybchinsky,
Dokt.Akad.Nauk SSSR, 1301, 1960; "Artificial Earth
Satellites", Vol.6, 101, The Publishing House of the
USSR Academy of Sciences, 1961.
17. W.Beller, Missiles and Rockets, January. 29, 1962.
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// NATIONAL REPORT OF THE USSR ACADEMY OF
SCIENCES ON THE INVESTIGATIONS OF OUTER
SPACE CARRIED OUT IN THE SOVIE'T UNION IN 1961.
h% Aeedemlei= A. A. Blagonravov 1L) 4
High Atmosphere and Outer Space
1. Rocket Investigations
In 1961, 113 sounding rockets were launched in the Soviet Union (see
the table).
During almost all the launchings the temperature and pressure measurements
were performed and the wind velocities and directions were determined.
The rocket launchings were used for studies of the regime of the stratosphere
over the mainland and the Pacific Ocean. The annual temperature, pressure and
density variations were investigated.
As a result of the investigations of the regime of the stratosphere over
the Pacific Ocean the conclusions have been drawn on the retention of the
continental thermal influences in the stratosphere, on the retention of the warm
Aleutian anticyclone up to heights of about 40 km and the stratosphere tempera-
ture field horizontal inhomogeneity. In the stratosphere the existence of the
constant easterly winds in an extensive tropical zone and also of the easterly
wind anomalous band has been revealed in the stratosphere in winter. The
scheme of the seasonal reconstruction of the circulation regime has been in-
vestigated.
The investigations of the total solar eclipse on February 15, 1961, have
been made by means of two sounding rockets. The program of observations
envisaged the studies of the outer solar corona and also of the state of the
upper atmosphere during the total eclipse and the moments close to the total
phase. The data have been obtained on the passage of the outer corona radia-
tions through the Earth's atmosphere.
In 1961 data were obtained for the first time on the neutral composition
of the atmosphere up to heights exceeding 300 km. During these investigations
helium was detected in the upper atmosphere at altitudes higher than 300 km.
The investigations of the ionic composition have led to the discovery of ions
of extraatmospheric origin at heights of about 100 km. Interesting data were
obtained on the intensity and heights of ,gloving layers in the upper
atmosphere.
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II. The Venus Probe
On February 12, 1961, the Venus probe was launched in the Soviet Union.
A new principle of placing a space vehicle in an interplanetary orbit was
used, namely, the launching of a guided space rocket from a heavy artificial
earth satellite. Such method of launching has opened up new possibilities for
interplanetary flights since the necessity is excluded of choosing the definite
time spans for flights to the Moon. At the same time the possibility is opened
of launching heavier space vehicles to Venus and other planets, limitations
are removed connected with the fact that not all launching points on the Earth
are favourable for the realization of flight.
The satellite with a space rocket aboard was placed in a nearly circular
orbit with the perigee 222 km and the apogee 280 km.
The space rocket was launched from the satellite in the precalculated
point of the orbit. When this rocket flight velocity relative to the Earth
became greater than the escape velocity and the rocket entered the precalculated
point in space its motor was switched off and an automatic interplanetary
station separated from it.
The creation of a powerful rocket carrier in the Soviet Union and the use
of the take-off from a heavy satellite have made it possible to place the
automatic interplanetary station with the weight of 643.5 kg in an interplanetary
path.
The automatic interplanetary station left the sphere of the Earth's action
and entered the elliptic orbit around the Sun.
This orbit is characterized by the following values: the maximum distance
from the Sun is 151 million kilometres, the minimum distance from the Sun (the
distance in the perihelion) is 106 million kilometres.
The automatic interplanetary station represented a unique space vehicle
and was equipped with the following apparatus: a complex of radiotechnical and
scientific instrumentation, the orientation and control systems, program
devices, the thermal regime regulation system, the power supply system including
solar batteries.
The radiotechnical complex of the Venus probe performed the following
functions:
Measurements of the parameters of the station motion with respect to the
Earth;
transmitting to Earth the results of measurements made by means of the
probe scientific instrumentation;
transmitting to Earth the information on the work of the probe instrumenta-
tion, on the pressure and the temperature inside the probe and on its body;
reception of radio commands of the Venus probe operation control from
the Earth.
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The control of the work of the instrumentation aboard the probe was
carried out by means of command transmissions through the radioline from the
ground points and also by means of self-contained programming devices aboard
the probe.
The probe orientation system performed the following functions during the
flight:
the removal of the arbitrary rotation caused by the separation from the
space rocket launched from the heavy satellite;
the Sun seeking from any position of the station and the orientation of
solar batteries to the Sun during the whole period of the flight;
the ensuring of any necessary spatial turn and stabilization;
the orientation close to Venus of the sharply directed (parabolical)
antenna in the direction towards the Earth to get higher speed of the transmission
of scientific information and data on the work of the Venus probe instrumentation
to Earth.
The automatic interplanetary station was equipped with scientific instru-
mentation to conduct physical measurements on the Earth-Venus path among them:
measurements of cosmic rays;
measurements of magnetic fields in the range from a few gammas to
several tens of gammas;
measurements of the charged particles of interplanetary gas and solar
corpuscular streams.
The processing of the results of trajectory measurements obtained during
radio contacts with the Venus probe has shown that the probe control system
ensured high accuracies of the placing of the automatic interplanetary station
in a flight trajectory to Venus. The calculated errors lay within the limits
of calculated tolerances of the control system errors. Without the correction
of the trajectory the Venus probe passed at a distance of about 100,000
kilometres from the surface of Venus.
The data obtained during the radiocontacts testified to the normal work
of the instrumentation and equipment installed aboard the Venus probe. The
orientation and thermoregulation systems operated normally. The temperature
and pressure inside the probe was within prescribed limits. The solar battery
charged current corresponded to the calculated one.
The scientific instrumentation during the radio contacts functioned
normally. New data have been obtained on the physics of outer space.
On the Venus probe traps were installed oriented to the Sun, one of which
was designed for recording the solar corpuscular radiation ionic component.
During the radio contact on February 17 it was recorded that the Venus probe
passed through a considerable corpuscular stream with the density of the order
of 109 particles per cm2 per second. This observation coincided with the ob-
servations of a geomagnetic storm. Such experiments pave the way for
establishing quantitative relationships between geomagnetic disturbances and
the intensity of solar corpuscular streams.
Laboratory experiments with the irradiation of three-electrode charged
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particle traps by electron fluxes have shown that such traps record electrons
with energies on the order of tens of Kevs very efficiently. These experiments
confirmed the correctness of the conclusion drawn at the beginning of 1960
by the Soviet investigators that the estimates of electron fluxes in the
outer radiation belt which had been made on the basis of the cosmic ray counter
indications exceeded the actual value by three orders of magnitude.
The Venus probe traps did not record considerable negative currents
during the passage of the Venus probe through the outer radiation belt which
confirmed once more the above-mentioned conclusion on the values of electron
fluxes in the outer radiation belt.
The Venus probe was equipped with more sensitive magnetometers than
those used on Soviet Luniks.
Information has been obtained during the two radio contacts with the Venus
probe: on February 12 on the magnetically quiet day and on February 17 when
magnetic disturbances took place.
The data of observations made on February 12 on the Earth and outside the
Earth's magnetic field at a distance of 165,000-175,000 km, have shown in the
main coordinated magnetic field variations relative to the average level within
the limits of 4 gammas.
During the radio contact on February 17, whose duration was about 15 minutes
the invariable value of the magnetic field was obtained. At the same time
terrestrial observations recorded the magnetic field variations within the
limits of 20-25 gammas.
One could not expect the close similarity of the curves, but in this
case one reveals the complete absence of simultaneity in the magnetic activity
on the Earth and in outer space.
The First Manned Flights Into Space
April 12, 1961, witnessed the great event. For the first time in history
man realized space flight. The space ship "Vostok 1" piloted by the cosmonaut
Yuri P. Gagarin was placed in earth satellite orbit.
The design of the spaceship Vostok 1 was based on the experience gained
in the launchings of the first Soviet spaceship satellites which made it possible
to work out the design of the spaceship-satellite and all its systems aboard.
The first three spaceship-satellites were launched in 1960, and spaceship IV
and V on March 9 and 25, 1961. At these space-ship-satellites medico-biological
experiments with animals were performed.
The program of the first manned space flight was designed for one Earth
circuit. However, the design and the equipment of the ship have made it
possible to realize more prolonged flights.
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After the completion of the program of the flight before landing the
ship orientation in the definite direction was carried out by a special
system. Then in the prescribed point of the orbit the retro-engine was
switched. After reduction of the ship orbital velocity by the value required
according to the calculation, the ship was transferred to the descent
trajectory.
From the moment when the retro-engine was switched on to the moment of
landing the ship covered about 8,000 km. The duration of the flight on the
descent portion of the trajectory was about 30 minutes.
Since the equipment contained in the cabin was published in the press,
I mention the equipment only briefly.
The cosmonaut occupied an ejector seat in which he remained during the
whole flight and which enabled him to leave the vehicle if necessary.
The pilot cosmonaut wore a protective space suit which ensured preserva-
tion of his life and working capacity even in the case of the depressurization
of the capsule in flight.
Vostok 1 was equipped with the following systems:
n landing system,
radio apparatus for communications with the Earth,
an autonomous system recording the work of instruments, radiotelemetry
systems and various sensors,
a television system for observing the astronaut from the Earth,
instruments for recording the physiological functions of the body,
the retro-engine,
an orientation system,
a flight control system,
radio systems for measuring orbital elements,
a temperature control system,
electric supply sources.
The control of the apparatus operation was carried out automatically
by means of program devices aboard the ship and, if necessary, by the pilot
himself.
Control units, orientation elements, shutters of the temperature control
system, and the aerials of radio systems were mounted on the outside surface
of the vehicle.
The pilot's capsule is much roomier than the cockpit at an aircraft.
The capsule instrumentation ensured the greatest convenience for the pilot in
flight. From his chair the spaceman can perform all the necessary operations
connected with observation, communication with the Earth, flight control and
the ship control.
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The space pilot can land in the ship capsule. Such method of landing
was tested in Soviet satellite spaceship IV and V which carried test animals
in their capsules. A variant was also provided for in which the pilot is
catapulted with the seat from the capsule at a height of about 7 km. and is
landed by parachute. This variant was also tested in descents of satellite
spaceships with test animals.
For measuring the spaceship orbit parameters and checking the work of
its apparatus radio measuring and radio telemetry instrumentation were in-
stalled on it. The measurements of the ship motion parameters and the recep-
tion of the telemetry information during the flight were carried out by the
ground stations located in the territory of the USSR. The data of measure-
ments were transmitted automatically through the communication lines into
computing centers where their processing was carried out on electronic
computers. As a result of this in the course of the flight information was
obtained on the main orbital elements and further motion of the ship was
predicted.
The radio system "Signal" aboard the ship served for the ship direction
finding and the transmission of the part of the telemetry information.
The television system carried out the transmission of the spaceman's
image to Earth which made it possible to conduct visual observations of the
pilot.
The two-way communication of the space pilot with the Earth was carried
out by a radiotelephone system which worked in the short wave ranges (9.019
and 20.006 megacycles) and at ultrashort waves (143.625 megacycles).
The ultrashort channel was used for communications with the ground points
at distances up to 1,500-2,000 km. The communication through the short wave
channel with the ground points which were located on the territory of the
USSR as the experience has shown can be ensured on the largest part of the
orbit.
For the ship orientation in the case of manual control the cosmonaut
used the optical orientator which enabled him to determine the ship's
position relative to the Earth.
The globe mounted on the instrument panel provided the opportunity of
predetermining alongside the ship's current position the place of descent
after switching on the retroengine at the given time moment.
The stores of food, water, regeneration substances and the capacity
of the electric supply sources were designed for the flight of the 10 day
duration.
Measures were envisaged in the design of the ship which prevented the
increase of the temperature inside the capsule beyond the definite limit at
the durable heating of its surface.
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-7-
After successful orbit around the Earth the spaceship landed in the
prescribed locality in the vicinity of the Smelooke village of the Pernov
district of the Saratov region at 10 hours 55 minutes Moscow time (7 hours
55 minutes Universal time).
After his return from the space flight Y. A. Gagarin feels well. No
deviations in his health were detected.
Gagarin's flight has made it possible to draw the conclusion of a
paramount scientific significance on the practical possibility of the manned
space flights. It has shown that man can normally undergo the space flight
conditions, the conditions of placing in orbit and re-entry to Earth. This
historic flight has proved that under weightlessness man fully preserves his
working capacity, the coordination of movements, the clearness of thinking.
On August 6, 1961, at 9 hours Moscow time (6 hours Universal time)
the second successful launching of the spaceship-satellite Vostok 2 piloted
by Major Herman Stepanovich Titov was realized.
According to corrected data the minimum distance of the ship from the
Earth's surface (the perigee) was 183 km, and the maximum distance (the
apogee) was 244 km.
On August 7, 1961, at 10 hours 18 minutes Moscow time (7 hours 18 minutes
Universal time) the ship Vostok 2 successfully landed in the prescribed lo-
cality over the territory of the Soviet Union near-the little town Krasny
Kut of the Saratov region.
For 25 hours 18 minutes of this historic flight the space ship covered
more than 700,000 km and orbited the Earth more than 17 times.
The design of the spaceship Vostok 2 was in the main similar to that of
Vostok 1. But on Vostok 2 a new more perfect regeneration plant was installed
which differed from that of the ship Vostok 1 by the composition of blocks
and chemical reagents.
The flight was planned for 17 circuits around the Earth. However, the
ship design, the store of food, water, reagents of regeneration system,
electricity supply sources enabled Titov to realize a more protracted flight.
After the placing in orbit the ship separated from the rocket-carrier.
During the orbital flight the apparatus aboard the ship worked according to
a program.
The description of the flight will be presented by Titov himself at this
Symposium.
The main and most important outcome of H.S. Titov's flight proved the
possibility of the complete retention of man's working capability during the
25-hour state in outer space.
The results of medical-biological investigations during the flights of
spaceship-satellites Vostok 1 and Vostok 2 will be presented in other papers
by Soviet scientists.
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By means of the series of instruments aboard spaceship satellites I and III
the energy spectra of various groups of nuclei, the chemical composition of
cosmic rays, the nuclear component variations and some radiation effects were
investigated. New data were obtained on the nuclear component flux short time
increases connected with the solar activity. For the first time such increases
in the nuclear component were recorded during Lunik II flight. This phenomenon
is characterized by a sharp short time increase of the flux of nuclei which
practically takes place simultaneously with the observed solar flares and radio
emission outbursts.
The energy spectra were obtained of various nuclear groups on the basis of
the measurements of the latitude effect. The nuclear spectrum was determined
from the charges in the range from alpha-particles to oxygen. At heights
200-300 km the enhanced radiation intensity was recorded over the whole surface
of the globe as compared with the intensity of the primary flux of cosmic rays
and data were obtained on the spatial distribution of the radiation intensity
at these heights. The fact of the existence of the increased intensity at
heights of 200-300 km agrees with the data obtained by the other group of Soviet
investigators and also with the data obtained in the U.S.A. and Japan, by means
of the Explorer 1 satellite about the increase of the radiation intensity in
a height range of 300-500 km as compared with the level of the cosmic ray intensity.
The detected gigantic anomaly of the radiation intensity at a height of
340 km over the southern part of the Atlantic ocean called the South Atlantic
anomaly and the radiation intensity anomaly at heights of 190-340 km near the
shore of Antarctic Continent called the South anomaly are connected with the geo-
magnetic field anomalies and apparently represent specific sinks of the particles
from the radiation belts.
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-9-
All these measurements enabled us to make more precise our conceptions
on the behaviour of the radiation belts near the Earth and to enlarge our
knowledge of the Sun as a source of multiply-charged particles of cosmic rays.
SATELLITE OPTICAL TRACKING
In 1961 observations of satellites were conducted by 84 Soviet visual
tracking stations and by 23 photographic tracking stations. In total 37 objects
were observed with the brightness up to +9 stellar magnitude, among them many
Soviet satellites: Sputniks 1960 v1 , 1960 & (Sputnik IV and its capsule),
3
1961/ , 1961 1961 (Sputnik VII and rocket carrier), 1961
(Sputnik VIII - Automatic Interplanetary Station); American satellites, 196021
(Echo 1), 1959 , 1960 , 1961 (Explorer VII, VIII, IX), 19616 ,
1961' , 1961 , 1961 ~ , 196171" , 1961X& (Discoverer XX, XXI, XXIIi,
XXIV, XXVI, XXXIV), 1960 91 , 1960 n 19611V (Tiros I, II, III), 1960
1960 2 ,, 1961 0 (Transit IB, IIA, IV A), 1961 (Samos II), 1961
1961Ot c (Midas III, IV).
The main methods of observations were visual by means of tubes AT-1 and
TZK, and photographic with the camera NATA- 3 c/25. The accuracies of visual
observations were 00.1 in position and 0.1 sec in time. The accuracies of
photographic observations were 4"-6" and 0.005 sec respectively.
In 1961 the amount of accurate photographic tracking increased. Cameras
were installed with movable film which made it possible to take pictures of
fainter satellites with the brightness up to 5-6 star magnitudes. The calcula-
tions of accurate positions of artificial earth satellites in 1961 were carried
out on the computers in Moscow and Leningrad.
10,200 passages of artificial Earth satellites were observed. About
47.5 thousands of visual positions were determined, about 7,000 negatives were
obtained for the determination of accurate positions.
The main work on bettering the technique of observations was aimed at the
automatization of observations and the enhancement of the tracking accuracy.
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The processing of observations and the calculation of the orbital elements
were carried out by the Institute for Theoretical Astrotm,my.! of the USSR
Academy of Sciences. In 1961 systems of elements for some of the satellites
1958 cc2 1960 ,~, , 1960 1960 ,~ , were published.
The evaluation of the quality of visual observations of tracking stations
is made by the Astronomical Council of the USSR Academy of Sciences from these
elements.
Photometric observations were organised at a number of stations. A
correlation is established between solar flares and the changes of the satellite
photometric period.
In 1961 the Astronomical Council continued cooperation with foreign
satellite tracking stations. About 200 stations located in 17 countries regularly
sent the results of the observations of Soviet and American satellites.
In 1961 the following data were obtained from foreign states:
The Number of
Passages a~_
The Number of
observations
Soviet Sputniks
2,600!
9,300
American satellites
4,400
15,600
The Echo satellite and its details
6,800
38,400
TOTAL
13,800
63,300
With a view of exchanging the experience of the work of stations the
Astronomical Council publishes "The Bulletin of Satellite Optical Tracking
Stations" in which articles are published on the problems of the techniques of
observations and the results of the processing of observations. The results
of the precise photographic observations are also published in this bulletin.
In 1961 the precise photographic positions were published for the satellites:
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Name of the Satellite Number Cofobservations
c.arcs=~=axa=:a.c
1958
1958
1960 ',
1960
1960 ~g
1960 Z
1960
During 1961, the results of the researches were published in several
magazines. The list of 156 publications will be handed over to the Secretariat
of COSPAR.
THE PLANS OF SCIENTIFIC INVESTIGATIONS FOR 1962
The program of investigating the upper atmosphere and outer space will be
continued. In the course of 1962, a series of launchings of artificial earth
satellites will be carried out.
The following phenomena will be investigated according to this scientific
program:
the charged particle concentration in the ionosphere, which is important
for studies of radio wave propagation;
corpuscular streams and low-energy particles;
the Earth's radiation belts composition;
the geomagnetic field;
shortwave radiation of the Sun and other space bodies;
the upper atmosphere;
the influence of meteoritic matter on the elements of the design of
space objects;
the distribution and production of cloud systems in the Earth's atmosphere.
The four satellites of this series "Cosmos" were launched early in 1962.
Medico-biological investigations will be continued during the next manned space
flights.
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APPENDIX I
Research Rocket Launchings in 1961
Place of Launching
The High Latitude Middle Latitudes
Observatory on of the European
Franz-Josef Land Part of USSR
January
February
March
April
May
June
July
August
September
October
November
December
Expedition The Total
Ships in the Number of
Pacific Launchings
4 4
8 9
13 22
*Among them two rockets were launched in the period of the total solar eclipse
on February 15, 1961.
**Research rockets for complex investigations of the upper atmosphere on
September 23, 1961, to a height of 100 km and on November 15, 1961, to a height
of 430 km.
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APPENDIX 2
SOVIET SPACESkIPS=SATELLITES, SPACE PROBES AND EARTH- SATELLITES
LAUNCHED IN 1961
S~at?llit~s
gattk
Artificial
Date
of
Launching
The Lifetime
of the
Satellite
Weight
The Perigee,
the Apogee,
the Period,
the inclina-
tion
(1)
(2)
(3)
(4)
February 4,
to February
6,483 kg
223 km
1961
26
328 km
89.8 min
64.6?
February 12,
to February
--
222 km
1961
25
280 km
89.5 min
65?
March 9, 1961
--
4,700 k6
183.5 km
(the lift-off
248.8 km
and landing)
88.6 min
64? 56'
March 25, 1961
--
4,695 kg
178.1 km
(the lift-off
247 km
and landing)
88.42 min
64? 54'
April 12, 1961
--
4,725 kg
181 km
(the lift-off a
t
327 km
9h.07 min, the
89.1 min
'
0
landing at
57
64
10 h.55 min)
(5)----_-~~s~a=m==
The test of the systems of
launching and the precise
trajectory check.
The launching of an automat-
is interplanetary station to
Venus from the satellite.
The testing of the ship de-
sign and its systems aboard
to prepare the manned space
fli,;ht. Medico-biological
experiment (the dog Chernush-
ka). Successful descent
and landing.
Testing of the ship and its
systems aboard to prepare the
manned space flight. Medico-
biological experiment (the
dog Zvyozdochka). Success-
ful descent and landing.
The first manned space
flight in the world and
successful landing at a
prescribed area. Pilot
cosmonaut Y. A. Gagarin.
Radio communication on
frequencies 19.995 Mc,
9.019 Mc, 20.006 Mc,
143.625 Mc.
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APPENDIX 2 (Concluded)
2=-=========
August 6, 1961
9h.00 min--the
lift-off; August
7, 1961, 10h.18
min--the touch
down
February 12,
1961
4,731 kg 185 km The second Soviet manned
244 km space flight and successful
88.46 min landing in a prescribed
640 56' area. Pilot cosmonaut H. S.
Titov. Radio communication
on frequencies 15.765 Mc,
19.995 Mc, 20.006 Mc,
143.625 Mc.
643.5 kg- Towards Venus. Investigation of interplan-
the weight Reached Venus
at the second etary ionized gas and of
of the half the
May, solar corpuscular radiation.
Automatic Invests ti f
h
etary
e radia-
1961. The min- ga ono t
Interplan- imum distance tion belts and of space
to Venus was radiation. Magnetic meas-
100,000 km and urements. Investigations
the distance of Meteoritic Dust. Radio-
covered 280 communication on 922.8 Mc.
million km.
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/,2
0.1. GOLYSHEV, A. M. BOROVICOV, G. A. KOKIN
y= (05
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/2
to
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hww
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BOCXOIlQt~ABEreb HHCXQcl~IAg efrBb
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I
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d/ A. E.IMIKIROV
.T7. AEROSOLE SCAT2ERING COEFFICIENT MILASUREI,IENT AT THE
The measurements of the sky brightness distribution
at altitudes is of great interest both from geophysical and
practical points of view.
It is common knowledge that the sky brighness in the
upper atmosphere is the combination of both the atmosphere
J.;urainosity and scattered light. In the day-time atmosphere glow
itself makes negligible contribution to the total sky
brightness, produced mainly by scattering effect by gas
molecules and atmosphere aerosoles.
Such investigations can be carried out both by indirect
measurements /twilight method/ and direct ones /vertical
atmosphere sounding by means of balloons and rockets/.
The day sky brightness investigation by means of rockets
began in 1946. In these experiments there were sometimes
used photometers, sometimes - photocameras. The.obtained results
give alternative data of day sky brightness.
Thus, for instance, Milly's experiments /I/ show, that the
sky brightness decreases with height and at the 35 km altitude
is of the order of 2-3% of the sky brightness near the Earth
surface.
At the 70 km altitude the sky brightness decreases 2 times
more and further remains constant up to the 135 km altitude.
On the basis of these data we came to the conclusion, thot
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a ,lie 135 In :altitude these exists luminous layer, the nature
of,-;hich is difficult to explain.
Bates and Dalgarno /2/ showed, that such -low cannot be
produced by the Earth atmosphere fluorecsence under the influence
of the solar extreme-ultravi?let radiation.
Other authors showed, that it cannot be explained by
zodiacal glow. Morosow V.M. and Shclovsky I.S. /3/ reject the
assumption, that it is the existence of the sufficient number
of aerosoles in the upper atmosphere, that causes this glow.
Berg's measurements /4/ have somehow slightly changed the
notion of the day sky brightness. According to their data the
day sky brightness at the 80 km altitude is 8.I0-5 stilb, i.e.
about 800 times more than the night sky brightness. Berg used
cameras for his measurements, however the measured brightness
was insufficial to make appreciable blackening on photoemulsion.
Based on this he made a conclusion, that at the 80-280 km
altitude the day sky brightness is 2.I0-5 times less than that
near the Earth surface. He found no luminous layers.
The latest experime:hts were performed by Birukova /5/ who,
like Berg, used cameras for the sky brightness measurements.
According to her data the sky brightness at the 56 km altitude is
5,2 epoetilb. If according to Fisenkova-Pjaskovsraja /6/, the
sky brightness near the Earth surface is 5000 apostilb, one can
conclude, that at the altitude from 0 to 56 km the sky
brightness fall I03 times. But at higher altitudes no'
measurements were taken by her. Thus,sufficiently precise
brightness value, and spectral energy distribution in the upper
atmosphere remained unlown.
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We measured the day sky brightness at different altitudes in
4 directions iby means of photoelectric photometer, designed and pi
produced in accord,,nco with the technical task of the Institute.
The apparatus is a high sensitive photoelectric photometer
with the viewing angle of the order of I00, the measurements
with it being taken by immediate comparison of the ex~ernal
radiation.signals with the standard signal,received from
luminous compound phosphor.
The apparatus block-scheme is shown in Fig.I. As can be
seen from Fig.I the apparatus optical scheme consists of
quartz lens, light filters, neutral absorbing filters, a concave
sperical mirror and a photomultiplier.
The apparatus is equipped with a device which allows to
agust automatically one after another light filters, a free
window, constant luminous compound phosphor and neutral absorbing
filters on the light beam way.
The device, is shown in Fig.I as 2 disks.
The neutral absorbing filters, included in the scheme,
provide for all filters, free window and luminous compound
phosphor to have sufficieily wide limits of the brightness value
variation, i.c. allows to make quite reliable mertsursments when
the measured value varies more thah I03 times.
The day sky scattered light, having passed the lens, the
light filter or the free window and the neutral absorbing;
filter gets on - to the spherical mirror, which sends'it to the
photocathode. FLU-25 is ua as the light rcceivor, with
sufficient Sensitivity it is the most stable, from he variation
point of view.
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For photornultiplier current am.)lification two cascade
amplifier of alternating current is used in the apparatus. The
light beam modulation is performed by rotating tooth disk,
fastened on electric engine axis. The anchor of electro-
magnetic genera or, giving reference, voltage for synchronous
detector, is installed on the same electric engine axis.
The apparatus provides for a contact, which gives an
impulse, thus fixing the beginning of each cycle of measures-
ments.
All above mentioned allowed to obtain, the apparatus
sensitivity of the order of O,SIO-8 stilbs for integral, light
and I,5.I0-1o 772 ------ for separate wave lengths. The neutr
cm stbI y.
al absorption filters included in the scheme widened the range
of the measured breightness from 0,5. 108 to 0,5.I0-5 stilbs.
The brightness of the constant luminous conpound phosphor
of different instruments was different and varied from
0,8.10-8 to 3,7.IO-8 stilbs.
The apparatus, described above was used for sky
brightness measurements up to 100 km.
A number of experiments was carried out for the
definition of the upper atmosphere brightness. The best
experiments from the point of view of the sensor optical axcises
disposition in space were experiment N4, performed in the
rpnthern latitudes, and experimbnt N6, performed in the middle
latitudes of the USSR.
The sun in the first case composed with the horizon an
in the
angle j3. = 1?50', andTecond case ao = 0?401. The results
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of the procesoing are given in Fig.2, where brightness values
in stilbs are plotted on the abciss and height in km - on
the ordinate. The curves clearly show, that in the middle
latitudes the sky brightness is more, than in the northeun
latitudes, ,.nd this can be accounted for only by the great
number of scattering particles.
For comparison Fig.3 gives the measured brightness values
and all known data, obtained by other authors. Besides, it
gives the sky brightness of absolutely clean atmosphere.
The brightness values, received experimentally, are
slightly higher than the Rayleigh ones. This may point to
the existence of aerosoles in the atmosphere.
As is known, according to experimental data the atmosphere
optical density can found from the equation.
,S s= sec g be f see ~e s~
- I/Ir (5)
where S0A - the source intensity before entering the
atmosphere;
f.~ - the intensity of the observed scattered radiation;
r~e 9)- the indicatrix of scattering,considering,gO) = (I-
cos2Y )
, what is quite 4cceptable for the scattering angle.
I800 120? , and assuming qtcos~y ca= b soa/t~sj,~/~a)
f6
where G...l - optical depth, corresponding to the Rayleigh
scattering,
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- optical depth, corresponding to scattering on the
particles according to Mie's law.
Thus, in order to determine the optical depth as the
Otatt?aY deptk as the Rayleigh one T , and as aerosole
component it will be quite enough to measure the scatter-
ed radiation intensity in 2 waves lengths or in 2 different
angles of the indicutrix of scattering.
For determination of the number of aerosoles in an
atmosphere layer it is sufficient to have the measurements data
of the scattered light brigtness at the upper and lower
boundary of the layer and then the aerosole optical depth of
the latter will be equal to difference:
?r Z
4J4 4, Z,
whence assuming of the layer x 60 J ~~ t 2/Va
`a.; J
one can define the value of aerosole scattering coefficient
where K(p) - Houghton-Chalker coefficient,
N - the number of scattering particles in I cm3.
r - the mean radium of a scattering particle.
Fig.4 gives J values for the nothern and middle
latitudes of the USSR. Besides, it gives scattering.ooefficient
values for absolutely clean atmosphere (fi ) for comparison.
The results , presented in Fig.4 , show, that from 80- to 100 km
there exists an aerosole layer with the maximum situated at the
85 km altitude in the middle latitudes and at 92 km iii the
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noothern latitudes, the number of -.erosoles being greater in the
middle latitudes, than in the nothern ones.
By means of Fig.4 data one can measure the uerosole layer
concentration and density. Let us assume(K,) = 4 , in other
words, we shall consider, that scattering takes place on the
particles with the maximum scattering coefficient, what morresp
corresponds to r = O,4J" It means, that we give the estimate
of tl,e minimum acrooole substance quantity. If we assume sp ci.C
is denaity of uerosole substance to be equal to 3 g/em3, in the
layer maximum (for the middle latitudes) N = I.IO-3 I/em3,
J = 8.IO-16 g~cm3 and for them thern latitudes 0,6010-3
16 3
4,8.IO d/cm
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I. Miley H.A., Callengton E.H1, Bedinger J.L. -
Trans.Amer.Geophys.Union , 1953, v.34, N 5.
2, Bates D.R., Dalgarno A. - J. Amer.Ter.Phys., 1954,
v.5 (5/b) p. 329-334,
3. Morosov V.M., Chklovskii I.E. - Isv. AN SSSR, ser.
gebphys. N 4, 1956, p. 464-468
4. Berg 0. - J. of Geophys. Research, 1955, v.60, N 3.
5. Birjukova L.A. - Trudy TSAO, 1959.
6. Fisenkova-Pjaskovskaja E.V., Isv.AN SSSR, 1957.
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
I. c~~ip.Mr~ MMOO4Ie
g- 'r
jIIf,VM/ wryoo
4 O6S Onw.refa
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Ham.
a/~/a~p4Rt+Ve+~t~w~e .
TION&VOS. foo IV* "*P.
f-B/4/ A14NLVO
80
V !b
?o 18"a N .1
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A. A. POKHUNKOV.
GRAVITATIC AL ,SEPARATION, COMPOSITION AND STRUCTURAL PARAMETERS
OP THE ATMOSPHERE AT THE ALTITUDES ABOVE 100 KM.
The results of measurements of the Earth atmosphere neutral
composition, made with radio-frequency mass-spectrometer during
2 soundings of geophysical rpckets in the middle latitudes of the
USSR: in September, 1960 (night) and in November, 1961 (day) are
given. Gravitational separation of Ar and N2 gases is found. Accord
ing to the first sounding data the height of the beginning of
separation is about 110 km. The atmosphere temperature distribution
was measured up to the 210 km altitude for the night experiment
and 300 km - for the day-time experiment. During the night experi-
ment the distribution of relative and absolute concentrations of N,
01 and 02 was found up to the 210 km altitude. At the 100 to 210
km altitudes there was also estimated mean molecular weight,
pressure and density of the atmosphere.
The limitimg concentrations values of the following minor
admixtures in the atmosphere:Nl, NO,H2O1 OH, Hand He are given.
During the night experiment at the 100 and 130 km altitudes
magnesium oxide MgO of meteoric origin was detected,
At 00.56 local time, on September 23, 1960 in the middle
latitudes of the European part of the USSR a geophysical rocket
was launched to the 210 km altitude. During this sounding the
container, separated from the rocket, was equipped with a 5-cascade
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high sensitive radio-frequency mass-spectrometer (minimum
registered current 4'10-141 corresponds to partial pressure At
2
5.10-lOmm mercury column) with"rmass ranges from 1 to 4 and from
12 to 60 atomic mass units. Detailed technical characteristics
of the apparatus and the scheme of its installation on the
container are given in work (1).
Neutral composition measurements by mass-spectrometer were
carried out after the container separation at the distances up
to. a few hundreds of meters from the rocket.
The particularity of this experiment mass-spectra is the character-
istic inherent only in atmospheric components periodic modulation
of ion currents, produced by arbitrary container rotation in its
flight and by pressure head effect. While the experiment data
processing this circumstance allowed to take into consideration
desorption of the container surface. The spectra recorded the ion
peaks, corresponding to the gases with the following mass numbers:
1,2,12,14,16,17,18,28,29,30,32,34,36,40,42 and 44, which were
identified with H1,H2,C,H1,01, OH,H20,N2,N14,Nj5,N0,02,0a64018,
Ar36Ar40,M9 260,CO2 and N20, respectively. Besides at the 100 to
125 km altitudes during the ascent and the descent there were
recorded the gases with mess numbers 9 and 10, which finally are
not yet identified.
On November 15,1961 at 16.00 p.m. local time a geophysical
rocket was launched up to the 430 km altitude. Neutral composition
measurements in this launching were carried out with a-mass-
spectrometer, installed in the head of the rocket under the
separated nose cone. The used 5-cascade radio-frequency mass-
spectrometer does not differ from the,described in (1) and usect
in the night 'experiment of 1960 - one in sensitivity, resolving
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power and mass range.
The apparatus was put to operation and began to record
atmosphereN mass spectra at the 130 km altitude.
Some results of mass-spectrogramunes treatment on the ascent
of the free rocket flight tragectory, where all the angles of
attack of the apparatus remained equal to 0?, are given below.
Gravitational separation.
The study of Ar and N2 ion currents ratio variation with
height in both experiments, presented in Fig.l, shows, that
both in the night and day atmosphere there is gravitational
separation of these gases. The comparison of these ion currents
laboratory ratio, corresponding to Ar content in the ground'
layer, with the values, obtained during the sounding, taking
into consideration the mass selection coefficient (2), shows,
that gravitational separation in the night atmosphere begins at ;ii
the 105-110 km altitude.
As for the day atmosphere the direct definition of this
level turned to be difficult due to the measurements being carried
out at the altitudes above 130 km, where, as can be seen from
Fig.l, there is an appreciable separation of Ar and N2. The
obtained results are in agreement with the data of 2 experiments,
performed in the mornings in summer of 1959 (3,4) in the USSR,
and also with the data of American authors, who studied the upper
atmosphere layers at 59?N (5). As to the conclusion of the
absence of gravitational separation in the atmosphere above
White Sands .(6) at 320N, one has to agree with B.A.Mirtov /7/,
doubting the. results , obtained by American authors, due to
unsatisfactory method of the experiment,
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Atmosphere temperature.
According to Dalton's law the barometric formulae is used for
gases concentrations distribution in the atmosphere above the
gravitational separation level, this formulae allows to compute
the atmosphere temperature and its variation with height according
to the scale height H=RT/Mg of any component.
The absence of the container orientation in the night experi-
ment of 1960 determined the. computation method. The temperature
was estimated according to the steepness of the slope of Ar and
N,, ion currents ratio variation curve (Fig.l), as this ratio
variation with the accuracy to the proportionality coefficient
is equal to Ar and NL relative concentration variation. The scale
height H=RT/(M MN)g was found according to the slope steepness
for the barometric formulae defining Ar and N2 relative
concentration variation with height. The temperature was
estimated in this way up to the 185 km altitude. From 185 to 210
km the temperature was estimated by linear extrapolation. The
errors of the temperature definition make up about 10% of the
me2~sured value. The estimated values of the night atmosphere
temperature are listed in Table 1.
As during the day experiment of 1961 the instrument orian -.ticr.
was constant (angle of attack=0?), the temperature was computed
from the curve inclination of N2 ion current variation (Fig.2)
which characterises the atmosphere nitrogen concentration
variation with height. The calculation of the velocity head gives
the following formulae for the scale height, from which the
temperature was estimated:
~ _ )
N = Hlo h?, Po
where HO- the scale height for N9 concentration variation
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i.ri ide %,ass-spectrometer analyser, estimated directly from the
Ccc>priess of the slope of N2ion current variation curve (Fi.2),
hm=430 km - the maximum height of the rocket ascent, h- the
height, where H0 was measured.
Temperature values are in agreement when Ar ion current
variation with height is used. The atmosphere temperature
computation was limited in this experiment to the 300 km
altitude due to the effect of desorption from the rocket becoming
appreciable at higher altitudes. The obtained day atmosphere
temperature values are also listed in Table 1.
The main composition, pressure and density
of the atmosphere,.
According to the data of 2 experiments, carried out at the
altitudes above 100 km the main components, determining the atmoei
sphere density are N21 01 and 02. In the altitude range l0L to
150 km there were recorded the isotopes N2(N14+ N15) with mass
number 29 a.m.u., and at the 100 - 126 km altitudes - the isotopes
02(06. 018) with mass number 34 a.m.u.
Relative concentrations of these isotopes at the observed
altitudes are practically constant and equal to (7,6 ? 0,6) x10-3
for N2 and (4,1 + 0,6) x 10-3 for 02, respectively, what is in
good agreement with ralative spread 7,6.16-3 for N14?N15 isotope
and 4.10-3 for 016.018 isotope (8). The study of the atmosphere
composition by means of mass-spectrometer at the altitudes,
where there exist chemically active atomic components, which can
partially recombinate or combine with the analyser inner walls
material, presents appreciable difficulties.
In work (1) on the basis of comparison of the experiments,
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perfor.ned with mass spectrometer analysers of different desiijs,
there was received the correction factor, which takes into account
possible reactions inside the analyser, which change the analysint
gases composition. By means of the night experiment data with
due regard for this factor there were obtained concentrations
of the main atmpsphere gases: 01 0e and N2 and the mean molecular
weight of the air in the altitude range 100-210 km was estimated
(see Table 1).
Using the laboratory data of N2 ion current variation with
partial pressure inside the analyser there was estimated N2
pressure at the 210 km altitude (excluding the background of
gas separation from the container) in the hight experiment.
Due to absence of the data of the container orienttion during
the flight, N2 pressure distribution in the altitude range-
I00-2I0 km was estimated according to the barometric formulae with
the use of atmospheric temperature values, estimated in the same
experiment. The obtained N2 pressure distribution is shown in
Fig.3, curve 2. Further computations with the use of 01, 02 ana
N2 relative concentrations data allowed to find the distribution
of the main atmosphere gases absolute concentrations, night
atmosphere pressure and d4neity at the 100-210 km altitudes. The
results of these computations are listed in Table I.
As in the day experiment of 1961 the mass-spectrometer
analyser had no shielding grid with positive ]potential,
contrary to the mass-spectrometer in the *llght experiment of
19609 aloiide with neutral particles it recorded atmospheric
ions, passing freely the ion source region. This resulted in
the fact that neutral atmmio oxigen could be found inspectro-
grammes only of the 130 to 160 km altitudes, and at 160 to, 430 la
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t;ie main part of the ion current was produced by atomic oxygen
atmosphere ions. In the altitude range 130-160 km OI and N2
ion currents ratios. are equal in both experiments. This
testifies to. the fact, that in view of different analysers
designs atomic oxigen relative concentration at the 130-160 km
altitude is slightly higher in the day experiment, than in the
night one. The aim of the,further treatment of the day
experiment materials is quantitative verification of 01, 02 and
N,, relative concentrations values.
As to atomic nitrogen N1, its concentration in the night
atmosphere at the 100-210 km altitude does not prevail 1-2%
of N2 concentration.
According to the extrapolation computations, made on the
basis of the obtained data by means of the barometric formulae
N2 plays the predominant role in atmosphere density up to about
280 km where the equality of densities JO(/! =J0 (Q,> is
observed.
Minor admixtures in the atmosphere
Helium. In the limits of the apparatus sensitivity after
the opening of the analysers neutral He was recorded in no
spectra, what allows to affirm, that at the altitudes above 100km
He concentration does not prevail 6x I07 particled/cm3.
H209 OH9 HI and H2 According to the night experiment data
H90 ion current variation pattern decreases with height and is By
symmetrical relative to the top.
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As can be seen from Fi;.4 H2O ion current modulation,
produced by the change of inlet position relative to the
contrary inflow is slightly pronounded in comparision with
N2(Fig.3). This points to the fact, the apparatus records mainly
H20, carried to the upper atmosphere layers on the container
surface. The maximum value of H2O partial pressure in the upper
atmosphere, estimated according to the ion current modulation
depth does not prevail 3?IO-7 mm mercury column at the 115 km
altitude, or 0,6% of the total atmosphere pressure. This value
must be cosidered as the upper boundary of H2 0
0 -content in the
atmosphere, as ion current modulation can be produced mainly
due to the increase of the number of H2O reflected molecules,
enering the analyser when the latter changes its orientation
relative to the contrary flow.
Hydroxile OH recorded by the mass-spectrometer with the
curacy tot the measurements errors is produced by H2O
dissociation in the ion source of the apparatus, what is confirmed
by the agreement of laboratory and flight ion current ratios
values ~~aN)/~(~.c~> ?
Thus, assuming the measurements error value to be the upper
licit of OH content in the atmosphere, we find, that the content 0
of hydroxile OH at the altitudes above 100 lm does not prevail
6?I0-3% of the total atmosphere pressure.
HI ion current pattern has analogous with H2O and OH
character of variation with height, what points to the
dissociative connection of HI and H 20 (Fig.4).
However,, beginning from 145 km HI ion current decreases
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slo,%,er, than it is necessary icr maintaining laboratory relation
of ion currents 5(H,O) I I(OH): 114I, HI concentration
at the altitudes above 150 km, corresponding to excess ion
current, is about I08 particles/cm3. This excess of 1I1 does
not contradict to the explanation of its existence by atmosphere
hydrogen, but final conclusions demand some additional
experiments to be performed: Apparently atomic hydrogen H
recombination inside the analyser fully accounts for the form.-:-
.ion of molecular hydrogen 1I20 found at the altitudes up to 1301:n:,
what is backed by HI and 112 ion courrencs correlation. As a
result of this, in the absence of H2 in the sp3ctra at the
altitudes above 130 Icm, the upper, limit of H2 concentration in
the atmosphere above 100 gm will give the value of 3-I07
particles/cm3.
NO. At the 130-180 Icm altitudes during the night sounding
there was recorded negligible quantity of neutral nitrogen oxide
NO. Its concentration did not prevail O,IJ of N2 concentration.
As the appreciable part of NO+ ions could be formed inside
the analyser as a result of charge-transfer reactions of the
following type: 0* + N2 = NO + + N, the given value can be consider-
ed to be only the upper limit of NO ccncentration in the atJ..ospherE
at the I30-ISO km altitude.
Atmospheric admixture of extra-terrestrial origin.
During the night experiment ascent and descent of the rocket
at the 103-126 km altitudes there was detected gas with macs
number 42 , indentified with the oxide of ML:; isotope, i.e. 1;:G20.
The oxides of 2 other isotopes with rna,ss,numbers 40 and 41 cannot
be singled out on the spectrogramnes due to the following reasons:
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The ion peak of the main oxide Mg240 was recorded simultaieonely
with Ar ion current, which was an order of madnitude more than
Mg240 amplitude. And Mg250 ion peak coincided with hegative
impulse from Ar ion peak /due to the amplifier super correction/.
Mg260 and N2 relative concentrations variation is shown
in Fig.5. Absolute concentration of all Mg oxides, obtained with
the consideration of their'relative distribution is equal to
about I'IO 9 particles/cm3 at the 103-126 km altitudes. Stone
meteors, where MgO content can be up to 40,2% of the total
weight, are apparently, the atmosphere source of MgO /9/.
At the same time stone meteors comprise the main part /860/
of all meteors, reaching the Earth /10/ from the point of view
of their weight.
MgO can be formed in the atmosphere in two ways. One part
of the molecules originates as a result of direct meteor
evaporation and the other - when vaporised Mg atoms oxidize in
the atmosphere.
Therefore the absence of metallic Mg in the spectrograiames
is explained M both by very small (0,03%) quantity of Mg in
metallic phase in meteor substance content (II) and by the
existence of considerable quantities of atomic oxigen , with whict
free Mg can combine at the 103-126 km altitudes.
Mg260 relative concentration decrease bbove 117-118 km is
in agreement with gravitational separation of gases at the
altitudes above 105-110 km. The decrease of relative
concentration below 117 km can be accounted for by the existence
of an extensive layer transitive from the atmosphere with
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the diffusion pattern of mixing of the -ases.
In this transition layer the gravitational separltion which
is just beginning is partially disturbed by separate flows from
the turbulent atmosphere, laying below. As to MgO, this
sircumstance leads to the fact, that MgO concentration in this
transition layer from 105-110 km to 117-118 km will decrease on
the account of partial mixing with the atmosphere layer, situated
below the layer of total meteor evaporation and therefore not
containing MOO.
The author is greatful to B.A.Mirtov for the usefull
discussion, A.A.Perno, R.F.Starostina and G.I.Podsoblyayeva for
their help in the experiment procession and treatment of the raicaz
material.
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Fig.I - Ar rind N0 ion currents ratio variation with hei-ht.
2
I and 2 - ascent and descent of the flight (ni ;nt,1960),
3 - ascent (day,196I).
Fig.2 - Variation of N2, 03, 02 and Ar neutral gases ion
currents on the ascent during the day experiment of 1961.
Fig. 3 - I - d, ion current variation with height of the ascent
with different orientations of the mass-spectrometer
(hight,1960) 2 - N2 pressure variation in the atmosphere
connted according to the barometric formulae.
Fio.4 - H20, OH9 HI and H2 ion currents variation with height
(time) on the ascent of the flight.
Fig.5 - Mg260 relative concentration variation with h&ight on
the ascent dnd descent of the flight.
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1. A.A.POKHUNKOV - Iskusstvennye sputniki zemli, ed.12, 1962,
(in print)
2. A.I.REPNEV - Trudy TS A 0, ed. 29, 66-73, 1960.
3. A.A.POKHUNKOV Izvestija AN SSSR, ser. geofiz., No.11,
1649-1657, 1960.
4. A.A.POKHUNKOV - Iskusstvennye sputniki zemli, ed. 7,
89-100, 1961.
5. E.B.MEADOWS and - Proc. of the first Internat. Space Science
J.W.TOWVNSEND Symposium, Nice, 175-198, 1960.
6. E.B.MEADOWS and - J.of Geophys. Res., v. 61, 576, 1956.
.! , W. TOWNSEND
7. B.A.MIRTOV -Gazovyi sostav atmosphery zemli. Izd.ANSSSH
1961.
3. G.SIBORG,I.PERLMAN, Tablitsa izotopov, I.L. Moskva, 1956.
G.KHOLLENDER
9. L.G.KVASHA- Meteoritika, ed.14, 75-85, 1956.
10.B.U.LEVIN, S.V.KOZ- - Meteoritika, ed. 14, 38-53, 1956.
LOVSKAJA, A. G.STARKOVA
11. .PlODDACK N.W. NatUrwissenschaft, Heft 35,
757-764, 1930.
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Ta67Iz a I.
1940Y.
16 A eOm. H.
,
p
,
T
T
Ar,,
n (02)
n (D.) ..M
? K
? K
C 3
p~j
a. t 1l, u.
3
r1n -~ . N
_3
Cm
9
100
215
7,4.1012
1,8.1012
6,E.1011
27,9
2,5.10 4
0 IO
110
265
1,7.1012
4,0.1011
2,1.101,
27,6
6,4.10-5
1,1.10-10
120
325
4,8.1011 I
I,I.IOZ1
7,9.1010
27,2
2,3.10 5
1.I0 II
130 600
395
T
1,7.1011
3,8.1010
3,5.I0I~'
26,9
I,0.I0-5
1,1.10-II
140 770
490
7,6.1010
1,6.1010
1,9.1010
26,5
6,7.10 6
5,0.10-12
ISO 900
600
3,6.1010
7,3.10
1,1.1010
26,1
4;3.106
2,3.10 12
160 1000
715
I,9.i010
,6.I0'
6,5.I0-
25,8
2,7.10 6
12
1,2.10
170 1140
785
1,1.1010
2,1.109
4,4.109
25,5
1,8.10-6
7,5.10-I3
180 1I70
825
7,3.10
1,3.10
3,2.10
25,1
I,2.I0-6
4, 9.10 I3
190 1190
860
5,0.109
8,0.108
2,5.10
24,9
7,3.10
3,4.10 I.
200 1250
895
3,3.10'
5,0.IO8
1,9.109
24,4
5,3.10 7
2,4.10-I3
210 1290
925
2,3.10-
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I,5.IO9
24,1
3,8.10 7
1,6.10-1''
250 1380
300 1560
Q' 56m ;cc.. i ,,e.
S'e
i emCe2 1960
2 3
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ti 0.01t
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q6
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no
ISO 200
150 200
120
Pl0 h Kn
250 TttH
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7
4 ON EFFECTS PRODUCED BY A BOD CIO ING FAST
IN PLASMA"
ky Y.L.Alpert, A.V.Gurevich and L.P.Pitayevsky
Summary I.
1..Partiple Concentration Disturbance and
tha Electric Field in the Vicinity of the Body.
The work presented deals with a theoretical investiga-
tion of electromagnetic disturbances caused by a body, for
instance, by an artificial Earth satellite, moving in a plaeipa
(the ionosphere). The indicated problem is of considerable
interest for two causes.
Firstly, during measurements of the gas density, ion
and electron concentration, of the electric field, the tem-
perature and other parameters of the undisturbed medium by
means of artificial satellites on space probes around the
body surface, it is necessary to have an idea on disturbances
of these values caused by the body itself, which, as we shall
see, dan be very large and extend at a large (in comparison
with the body dimensions) region.
Secondly, of great interest is the investigation of
the electromagnetic wave scatteria on the perturbed _'egion --
on the "trail" of the body which is carried together with the
body along its orbit.
It should be also borne in mind that problems connected
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with the body motion in a rarefied plasma are very peculiar
and by themselves are of theoretical interest.
The satellite motion in a rarefied medium has been in-
vestigated by several authors. However, the majority of the
authors were interested only in the calculation of the fric-
tion force acting on the body (1). In some works the struc-
ture of the disturbed zone was studied (Kraus and Watson
(2), Rand (3) , and only for the case of a weakly char,ed body
with dimensions email as compared with the Debye radius. That
is why their results have no direct relation with the motion
of actual satellites in the ionosphere. Besides, using the
perturbation theory these authors dropped the term of the,
second approximation essential in this case. Therefore their
results are incorrect, at large distances from the body.
In our works we studied directly electromagnetic effects
produced under actual conditions by a satellite moving in
plasma (4-7). Some of the results obtained are given below.
In this complex of - problems of great interest is calculation
of a particle flux in the vicinity of the body. Besides,
the case is important when the body velocity becomes commen-
surate with the thermal velocity of particles or lower than
it, and the body dimensions become commensurate -~jith the
Debye radius, when the effect of the electric field,is es-
pecially significant. This takes place at the transition
into interplanetary space. However, the results of the
analysis of this problem have not been considered here.
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The body motion in the upper atmosphere usually takes
place in conditions when the particle free paths are large
as compared to the body dimensions, and the body interacts
with neutral molecules and atoms, ions and electrons. Since
V 8!c
it moves with a hypersonic velocity. V>> M
where ZMT = ?I7, is the mean thermal velocity of ions
and neutral particles, their concentrations around the body
are considerably perturbed.
In front of the body naturally an excess of particles
appears due to reflection of the incident flux from the body
surface. The "condensation region" is formed here.
On the rear of the body, to the contrary, the rarefabtion
region is formed since the body "sweeps out" the particles
and the latter have not enough time to fill this region com-
pletely, since Vt KT
that is considerebly exceeds their thermal energy e~p KT
On the contrary, the electron distribution is fully
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determined by the.electric field and for them the BoltWmann
distribution is always true. The main influence on ion
filling is exerted by the outer magnetic field which retains
particles hindering the filling of the rarefied region by
ions. The character of the filling and the rarefaction
region dimensions essentially depend on the angle between
the body motion velocity Vo and the magnetic field vector Ho
The solution of the above mentioned problems requires
kinetic consideration, since it is meant that the particle
freepath A is much larger than the linear dimensions of
the body Ro. In the coordinate system connected with the
moving body the particle distribution is stationary and
is described by kinetic equations
Paz 21M 0
Mazar
the =0
rj aze_ ~m m m~H,v+?;~ IT (2)
_ e t 1 +e [Ri 4i 0 (3)
az (M 8'c M 8i fic L y ~} 2u
In equations (l)-(3) fH(z,) , fe(z,~~ and
(z, U) are distribution functions of neutral particles,
electrons and ions, a is the electron and ion charge, m and
M are electron and ion masses,
=Y ) is the electric
field potential, H is the outer magnetic field LI=Zl~z--6t~
is the potential energy of the interaction of particles with
the body surface U=~~u . At infinity naturally
JM, ft and fe are Maxwellean functions. The electric field,
which is formed due to the difference in electron and ion
concentrations in the disturbed zone, is defined by the
-.
Poisson equation, d~=4ne fe(Z'Od 3U. (z, it) d3u)
with boundary conditions.
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- 5 -
Neutral Particle Disturbance
The distribution of neutral particles is determined by
equation (1). Its solution is obtained for mirror and dif-
fuse reflections of particles from the surface. For the den-
sity behind the sphere of radius 'Ro distribution 1j 9,2)
I'M.
is obtained presented in Fig.l for my; =8 . As seen
2xT
from the figure, the extended rarefaction region is formed
j5/ZMois
here, in which ti40Ro before the distance /I 4L
reached. The dependence of the particle density in the con-
densation region in front of the body for different jO and Z
at mirror reflection is shown in Fig.2. It is seen from the
figure that close to the body surface, the neutral particle
concentration is increased two-fold at a distance 0.2 Ro
from the body surface 5-- - 1.5 and at a distance of a
No -
radius - 1.1. With the increase of the distance from
the body surface the concentration disturbances in the con-
densation region decrease more rapidly than in the rarefac-
tion region.
The particle concentration distribution in the conden-
sation region at diffuse scattering is shown in Fig.3. In
this case the reflected particle concentration near the body
surface is much higher than in the case of a secular reflec-
tion. Let us note that since the velocity of the incident
particle flux is much larger than the therrial veloc~ty, the
collisions of particles filling the rarefied region with
the body surface are of little probability and at4arge
distances they weakly affect the particle concentration.
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This means that the concrete shape of the body in the rare-
fied zone at distances Z>> Ro is insi3nificant, of import-
ance is only the shape of maximum body cross-section in the
plane orthogonal to the incident stream. Corresponding cal-
culations for the body with a cross-sections lead to a very
simple and graphica.L formula 2 s z
SMuo e MV ~
nM 21rKT 2 (2KT ze (5)
Ion and l;lectron Disturbances
The set of equations (2-4) describes the ion and elec-
tron distribution functkns and the electric field. In the
general case it is very complex. However, taking into ac-
count that the Maxwell-Boltzmann distribution is true for
electrons it can be s olved
2ecclz) ,
N z N M e Mu #
e a ~2~rKT, 2KT
For ions as the first approximation the electric field effect
can be ignored.
With the magnetic field taken into account when l fli
for a circular cross-section of the body of radius Ro in
the plane perpendicular to the direction of the motion cue
obtain for the ion concentration in the rarefied zone
-u&
C , pu du (6 )
N (p, a)= Nw-2ND e.xp - 11P U e I ~C
S" Z.
/2
~" 2 J ~N .SrIL "
I PH 2- RoV2.p tJ" Zr.
Here ?H = is the romfa'Vgnetic frequency
MC
PH= e eH -/-X TM is the average Larmor ion radius, Io is the
Bessel function from an imaginary argument. From formula (6)
is evident that in the close zone the magnetic field effect is
of little importance as it should be. At 'TZ > If. the
H
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-7-
magnetic field effect is, to the contrary, very greatNt (p,8)
is a periodic function Z with a period = . In Pig.4
H
corresponding curves of equal values Ati(y,7)/N` are shown
for Ro-pn and 3 Vii, -$ . In this case the variation
A N
period
'
expressed in radii of the sphere Rol is
Neo
equal to 50.24. When the body moves orthogonally to
14( Not l1 ) the structure of the disturbed zone is more com-
plocated. The dependence of surfaces N.
= 0.8 for
PH 0.3 Rx and N = 0.93 for 5y- Rx on x, y, z for the
body of a square cross-section, when KT S is shown in
Fig, 5, 6. In' contrast to the case of the longitudinal body
motion (?la //f/ ) the disturbance does not remain constant
and decreases with distance as . Let us remind here triat
oN
in the case whenHH= 0 N decreases with distance propor
A Ai
tionally to z , while at H117 the ratio
does
N!o
not decrease at all with the increase of distance when the
collision frequency )=0
The Electric Field Around the Body.
Using the BoltOnann distribution for the electron density
we have the equation for the potential lj7(Z) around the body
N(~)-exC8K
where si (Z ) = ffd3U is the ion density, No is the
undisturbed electron density. Since we consider the case when
Ro >> D (D is the Debye radius), the solution of (7) gives
the following expressions for ((7) with an accuracy to the
terms "on the order of -L in the vicinity of the body
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and with an accuracy on the order of A
at a large dis-
tance from the body (A
~(z) ~ eKT &
1The distribution
j )
_ ..
D - T ((
o J? (8)
lli'av P
of the potential in the vicinity of
Qspherical body determined by formula (8) is shown in Fig-7.
Since in the ionosphere en A - 10, the potential cp in the
maximum rarefaction region is by an order of magnitude greater
than a i.e. (PI 1 volt. In front of the body (f , to
the contrary, is only of the order of a i. e.
14) '' 0 05*Q 1 volt.
Results of the calculation of tfl'z) for the body with a
metallic surface are presented in Fib.8. From the figure is
evident that the (P potential' variation close to the surface
(in the region of maximum rarefaction) has changed consider
ably as compared to the case of the reflecting sphere, as it
should be. However, the maximal value 4lis' as before,
61 In A. It is reached not close to the surface of the
e
sphere, but at a distance on the order of Ro from it.
The electric field which is formed due to the plasma
disturbance caused by the moving body is calculated above
ignoring the reverse effect of the electric field on the per-
turbation, i.e. on the ion motion. Actually this is of course
true only to Co first approyimation. It stands to reason
that the electric field affects the ion motion. However, as
already indicated above, due to a large ion velocity with
respect to the body, this influence is not predominant or the
problem considered here, since
MV,2>>e(p(z).
We have shown that with a strict -account of the electric
field in the general case, whenW= 0, the ion density
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disturbance decreases at a large distance from the body
proportionally toy , which coincides with the results
obtained above without the electric field taken into account.
This shows, in particular, that the results of Kraus and
Watson (2) who obtained the decrease ti J- are
erroneous.
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ON EFFECTS PRODUCED BY A BODY MOVING FAST
IN PLASMA"
Y.L.Alpert, A.V.Gurevich and L.P.Pitayevsky
Summary II
II. Radio Wave Scattering on the Body "Trail"
The electron inhomogeneity which produced around the
body leads to the scattering of incident radio waves. The
structure of the scattered electromagnetic wave field changes
in a complex manner depending on the angle between the incid-
ent wave and the direction towards the. observer, on the angle
between the magnetic field and the. body motion direction, on
the wavelength and plasma parameters.
At the scattering the body rarefaction region plays the
greatest role. Due to the influence of the outer magnetic
field, as we have seen, for instance, in the case of the mo-
tion along the field, the rarefaction region is of a cylindri-
cal form with a periodically changing surface 6) - const.
Along the magnetic field the length of this formation is on
the order of the ion free path. Its transversal dimension Ld
on the order of the limear dimensions of the body Ro or the
eI,M C
Since cases of artificial satellite or rocket motions in
the ionisphere or interplanetary medium which areaf actual
interest to us correspond to the case
A>>R0, (1)
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the theoretical calculation requires the solution of the
kinetic problem. Keeping in mind that frequencies usually
used satisfy the condition
W ?W (2)
(where c.)?=,eH,;p4 is the electron Larmor frequency) we can assume
and use, the perturbation method for the calculation of the
scattering at distances larger than the wavelength. The elec-
tric field of the scattered wave E' and the, effective scat-
tering cross-section in the element of the body angle dO
are as follows:
eP a KR~KfK,Eoll Ng (4)
E-mw R L J1
2
4AJQ
)~4K4 2 dO (5)
~-16Jr2e w/
(
In formulae (4) and (5) E and K are the electric field
amplitude and the wave vector of the incident wave, resppec-
tively, K' is the wave vector of the scattered wave, is
the angle between k and Co ,No is the undisturbed electron
density
NN(Q)= JdN()ep(-i)d, (6)
the Fourkier-component of the electron disturbance 8N(Z),
2K $&1 (7)
is the scattering angle (between K and k' ) and d3 is the
volume el eme nt .
The NIV function can be determined in a more straightfor-
ward way directly from the kinetic equation. This makes it
possible to solve the problem stricter and to take into account
the influence of the electric field and the collision frequency
E_ !- 44Ne2=I--~qio ,
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between particles which considerably affect the scattering
at distances from the body larger than its dimensions. This
region makes the greatest contribution to s a ter ng.
Let us determine the ion distribution function in the
(8)
Due to the fact that the body velocity is much lower
f(U,z)=J (u)+,f
3~p s
5(u) =iv0~2MKT~ exp(-2- )
than the electron velocity ( Vo?
), the electron
density is expressed by the Boltzmann formula:
N(z)=NoeapI L410T_ )J ' (9)
As a result of this, NV calculation reduces to the so-
lution of the kinetic equation for ions and the Poisson
equation which are written in the coordinate system, where
the body is at rest in the form:
o +p-C{LZi} u~+~~~1 NJ du eoso~,
L i z -~Qz
where J (~,u)- f e cpQ(l~,)=tie X z
The right side of equation (10) has the meaning
integral of collisions" of ions with the body and is
in assumption that all incident ions are neutralized
body (a metallic one). In this case we have:
Y(u) -1r R. Jo V,-
% yM0-sin O)dt~,
0
of "the
written
by the
(12)
where CM9 ~V and to is the Bessel function. The
0
effective collision frequency is introduced in such a form
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that the law of particle preservation should not be violated.
Then the collision integral Y has the form:
Y=-~(f No~fd u)=-~~f f'd u) (13)
As a result of the integration of (10) we have ulti-
m et e ly : _ 7R ~ex.o ' x 2MS?2 (Q~ X2f2) J
N-
%[2~ Jezyi{ ($x2)dam T~`"' 4J
S2 f 9 2MS12 1
where ,Q = MH , o (~, and % are longitudinal and transversal
components of 9, relative to the magnetic field H
It should be noted that though formula (14) is derived
as a general one, the effect of the electric field on the
right side of (10) is not taken into account with sufficient
consistency and the collision integral is also introduced
not rigidly. How essential it is can be found by a stricter
analysis which is very difficult to conduct.
Substituting (14 ) into (5) after some calculations we
obtain the differential effective scattering cross-section
in the coordinate system connected with the body in the form
? 2 =e)/2 (15)
~~z9 - NO
C '3 0.0
where ?) and t designations are evident from Fig.l,
is a bisector of 0the9 angle between
r3(a,,Py, ~, o l
(2-2,nP'-o'i) f(or 2,p F2')2
(16)
C'(- CYO = 4 (cos~stnO4-5vcz9eoszJCq), p- H, ~'-2s'
H 2 H K T 2 2 W 2/ CJo S.it2 `-h
a= AT , c211- c.w2) , 2
H
-3 ? X)tx
e f sr.?.~ exr
O
00
F'' = e s Je sax exp(-px-yx *Jcosx)dx ,
(17)
(18)
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-5-
The main features of the effective scattering cross-
section (1-5) are determined by the scattering function
) which was tabulated by us on an electro-
nic computer for three heights of the ionosphere
Z - 300,400,700 km.
Analysis of P
3 011 02, p) shows that depending on
angles O, , 19 and (F between and H , the normal R to Ho
and Q and planes ( Y H ) and is
a multilobe sharply directed function with the main maximum
(0) c = 0 at 2Y = 29 fl =0 . Lateral maxima and
minimal (+ 1 m , 12m ....) and (+ 1 m, + 2 m) correspond
to the values
?"max = + 1.22, ? 2.18, ? 3.15, ? 4.23
?'min = ? 0.73, + 1.70, ? 2.91, ? 3.86
As is evident from Fig.2,3 built for the case when
1 =0 for , = 30 m, = 300m, A35'~~) is
simmetrical with respect to the value a. = 0
(=ts =0 ). In this case does not depend on
Therefore, the plane P"Va2, V) is formed as a result of
3 (0s) rotation about the axis No (Fig.4). When O0
( 1o is not parallel to (d,J )(f ) is asymmetrical
with respect to t92 (Fig-5) and depends on 0 . The N
surface has already no axial symmetry (Fig.6).
When Z. /1.4 as can be easily noted, the main maximum
of the effective cross-section lies in the direction of the
mirrorreflection from N, , and, when 0, #0 , it is
turned with respect to this direction by the angle
determined from the equation=4. The main maximum (0)
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is the sharpest and considerably exceeds lateral maxima
which is evident from Table I. Effective
6' values which
correspond to the main maximum and their ratio to the overall
effective cross-section of an ideally conducting sphere we
given in the same Table for different wavelengths and radii
of the sphere Ro and also for the day and night ionospheres.
At daytime and, in a number of cases, at night, the effective
cross-section (0,0) of the " trail" main maximum con-
siderably exceeds the effective cross-section of the sphere
itself reaching many tens and hundreds of square metres. The
scattering increases with height in the range of 300-700 km.
With the decrease of the wavelength, 6 decreases fast
and at X45 m it is already small. Thus, at the point of
observation, as the body approaches, at first the scattered
field monotonously increases, then outbursts are observed due
to the lateral end main maxima, after which the scattered
wave intensity again decreases monotonously. Practically the
scattered field is sufficiently large only during several
~t =
time intervals 9'r For these time intervals
Y
0
sufficiently intense and narrow maxima pass distances
d'z - Z So
near the Earth where 2 is the body
height, and 89 is the maximum angular width. It is
natural that the effect of scattering from the "trail" is
revealed only under the condition when it is larger than the
scattering effect of the body itself or is equal to it.
This takes piece when the body moves close to the magnetic
field direction . Analysis of the effective scattering
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Gros -section hay e :o' n tact for the rr : ,ion of ionospheric
heights ..onsider.-.d here the width of the squwe "illumi-
nated" n,~ar the Earth's surface by diz'ferent lobes is
?41-9) km, the burst tii,iesa t4d ^x(0.2-1) sec., ai,d time inter-
vals between individual bursts At"' are (3-5) sec. It is
natur-il that if the r.,;iouu where the body flies is irra?ia-
ted fro a points (see at diffe.-ee.it an;;les, the
time of the action of the trail scatter'_nG effect is con-
sidernoly increased.
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Table 1.
Valu j1 -0 `/-O/ 1'~Q.K) (5,40K and ('
~s of ---9 ---------------
----- A -----------30 -----------------20-------------------15
------
300:
4001
700
300
400
700
300
400
700
--
P Mak
3,
/0/
53,46
134,4
1535
11,07
31,05
479,3
4,82
14,10
241,3
- ?
/1/
9,39
13,18
3,18
- ~-
/11/
0,89
1,15
0,62
- It --
/lil/
uuuc
-,:-
-7
--------Ro- ?- 1-m------------------------------------
--------~ -m2--15--- 26 30 3 5s6 0,8 1 2 4
day
Go
350
590
630
14
2:
36
1,6 3
5
(5
M2 0,05
2,6
4,6
10
2
0,6
1,3
3.10 3 0, 2
0,6
nisht
9
1.1
6U
9,6
5?l0
2
2,5
57
1072 0,3
0,8
-------------------------------------
Ro = 3m --------------------------------
-------------------------
-------- 6M2 810 1420 1620 98 184 280 18 35 60
dqy 28 50 58 1 2 2,8 0,3 0,5 0,8
0
-------- -2 2,7 142 240 0,3 18 50 6.10 35 9
niailt .10 4 0,05 0,8
0,1 5 8,5 4.10-3 0,2 0,6 7
--------- ----------------------------------------------------=---------
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(, 1,'\
by V.I.Krassovsky,
Institute of Physics of the Atmosphere,
USSR Academy of Sciences, Moscow
The atoms of nitrogen and oxygen,and,to a lesser
extent,those of hydrogen,carbon and chemically inert helium,
are the basic atoms of.the upper atmosphere. Despite,however,
the scanty assortment of atmospheric atoms and of their ions,
the compounds,and chemical reactions in which they participate
are rather numerous. An extensive,thouth far from complete,
list of possible reactions is given,for example in the well-
-known works by Bates,Nicolet et al. /1,2,3,4 and 5/.
More definite information has become available in recent
years regarding the electromagnetic and corpuscular radiation
of the Sun, which dissociates the molecules of the atmosphere
and excites and ionizes its atoms and molecules. Following
such primary processes, there begin complicated chemical
conversions, and there appears, figuratively speaking an
atom-molecular or ion-atom-molecular "kaleidoscope." But
modern data on the rates of the possible reactions are quite
uncertain and even contradictory. By way of illustration,
Table 1 presents data on the rate coefficients of some major
reactions in the atmosphere at altitudes from 70 to 100 km.
The vagueness of their values is too great. Much energy and
great efforts may be applied to compile and solve systems of
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JIf I'. CHEMISTRY OF THE UPPER ATMOSPHERE
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compound equations, but because of the above fact the final
result will not prove of any practical value. Many researchers
assessed the coefficient of the rate and of the energy of
activation of reactions in the atmosphere and in rarefied
gases under laboratory conditions, proceeding from a limited
number of processes under consideration. Such an approach
would be fully justified if the processes under consideration
were actually the only ones possible. With the existing
uncertainty with regard to the values of the reaction rate
coefficients it is impossible to specify reliably the most
likely processes of the upper atmosphere. In briefly review-
ing the present-day state of the chemistry of the upper
atmosphere, it is most advisable to stress the most contro-
versial points.
The principal data on dissociation of molecular oxygen
are collected in Table 2. The average daily flux of solar
radiation quanta dissociating molecular oxygen has a value
of the order of 1012 and ,xlO11 quanta cm 2 Sec-1 in
the Runge-Schuman bands and continuum respectively. In
polar regions, dissociation of oxygen and nitrogen molecules
may be considerably greater owing to the invasion of corpuscles,
especially during aurorae. Table 3 shows the process of
recombining atomic oxygen the w8.y it had been conceived before
hydroxyl radiation of the upper atmosphere was discovered.
After this event, however, Bates and idicolet /l/ and Herz-
berg on his own /14/ suggested a new mechanism according
to which oxygen molecules emerge from ozone molecules and
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3?
oxygen atoms through the mediation of atomic hydrogen which
is the catalytic agent. The scheme of such a process is shown
in Table 4. An oxygen molecule pair is formed in such react-
ions from the ozone molecule and the oxygen atom. For energy
considerations they account well for the maximum excitation
of hydroxyl only to the 9 vibrational level of the basic state.
Somewhyt later Krassovsky /15/ suspected thyt more excited
conditions of hydroxyl, exceeding this level, may be rapidly
destroyed below 80 to 100 km during collisions with oxygen
molecules as a result of which ozone and atomic hydrogen will
reappear. McKinley, Garvin and Bodart /16/ confirmed by
means of laboratory experiments the maximum oxcitation of
hydroxyl to the 9 level in an ozone-hydgogen mixture. It was
still to be clarified, however, to what extent this is due to
the ozone-hydrogen reaction itself, and not to the destruction
of strongly-excited hydrixyl by oxygen molecules.
Most remarkable proved to be the enormous power of hydro-
xyl radiation of the upper atmosphere. On the basis of a vast
observation material dealing with middle geographical latitudes,
Shefov /17/ determined the mean intensity of hydroxyl bands
in the visible and near infrared region of the spectrum.
Regretfully enough, the laboratory appraisals of the relative
intensities of the bands from the same levels, made by
Garvin, Broida and Kostkowsky /18/, led to results differing
from those obtained by Shefov. And yet, if one is to proceed
from Shefov's data and determine by means of interpolation,
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4?
taking into consideration the linear terms only in an
expression of the dipole moment, the intensity of more infrared
bands of hydroxyl in the region insufficient for observation,
as was done,for instance, by Shklovsky /19/ and, as a variant,
by Heaps and Herzberg /20/, it is possible to assess approcim-
ately the average yield of the newly-formed hydroxyl molecules
apart from optical transitions from higher states. It may be
appraised as loll cm -2 sec-1 for every vibrational level of
the basic state,beginning with the 9 level and lower. Thus
it may be expected that the total number of newly-formed
hydroxyl molecules on all the vibrational levels will reach
1O12?cm-2 sec-1. The number of such processes in the upper
atmosphere is greater than the number of destructions there
of oxygen molecules by Sun radiation in the Runge-Schuman
continuum; it is commensurable with the number of destruct-
ions of oxygen molecules by its radiation in the Runge-Schuman
bands. Although such an appraisal is somewhat vague, there
is still the impression that such a yield of new hydroxyl
molecules and, consequently, of oxygen molecules, even if it
does not exceed the number of dissociated oxygen molecules,
undoubtedly constitutes its important part.Reference has been
made here to the mean values of the hydroxyl formation rate.
Actually, however, considerable fluctuations of intensity of
this process take place. Greater intensity of hydroxyl
emission has been recorded at higher geographical latitudes
/21/.
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5?
After the appearance of the ozone-hydrogen hypothesis,
Kraeeovsky /22 and 23/ assumed that there exist other possib-
ilities for the appearance of hydroxyl radiation. According
to his suggestion, reactions referred to in Table 5 are
possible in the region where the radiation appears. It is
noteworthy that,according to this process,atomic oxygen, in
the main, passes into a molecular state not during the union
of two oxygen atoms in triple collisions, but as a result,
first of the formation from molecular and atomic oxygen in
triple collisions of ozone, and then of the reaction of ozone
with oxygen atoms. Krasoovsky stressed that metastable
vibration-excited oxygen molecules, incapable of being deact-
ivated by radiation, can be preserved for a long time and can
stimulate -diverse reactions with a coefficient of atomic ex-
change processes rate of the order of 10-10 cm3 sec-1.
Subsequently Norrish et al. /24/ reported on the prolonged
existence of such molecules observed by them under laboratory
conditions. The maximum excitation of hydroxyl to the 9
level Krassovsky explained by the fact that the vibrational
excitation of molecules is limited by the state sufficient
only to provide for the appearance of hydroxyl with an
excitation not exceeding the 9 vibrational level of the basic
state. More highly excited oxygen molecules are destroyed
during their collisions with non-excited oxygen molecules, as
result of which there spring oxygen atoms and ozone molecules
A similar process has already been referred to in Table 2
(process 2).
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6.
It has been ascertained by means of rocket investigat-
ions that a hydroxyl emission, emerges in a region whose
altitude and thickness change substantially. For example,
Parker /25/ made it known that a maximum intensity of this
emission was observed in one instance at an altitude of 80 km,
and in another case at an altitude of 90 km. Tarasova /26/
even reported about two maxima of hydroxyl emission intensity
near the same altitudes. Thus, hydroxyl emission appears
considerably higher than originally Supposed by Bates and
Nicolet /1/ and much lower than originally assumed by Kras-
sovsky /22 and 23/. At the time 'rassovsky /15 and 27/ noted
that initial acts of molecular oxygen dissociation, due to the
dissociating radiation absorbed there,are not sufficient for
hydroxyl emission to appear in a non-mixing atmosphere at an
altitude of 80 to 90 km. An ozone-hydrogen reaction can in
principle take place, however, at such an altitude if there
exists a vertical mixing of the atmosphere,which provides for
an influs of all the necessary initial products into the
reaction zone. To account for the high content of molecular
oxygen above 100 km, Nicolet /28 and 29/ took the vertical
mixing of the atmosphere into consideration. Inasmuch as the
temperature of the atmosphere considerably increases with a
decrease in altitude below the temperature minimum at an
altitude of some 80 to 90 km, very favourable conditions
exist there for vertical mixing. Simultaneously, owing to
atmospheric viscosity, a higher region of the atmosphere above
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the temperature minimum will also be involved in this
process. Actually circulation in the atmosphere is most
likely of a zonal nature. In some places there are up-
stream flows, in other downstream and in still other places
horizontal flows. In the region of the temperature minimum
there probably exist regions where there is a slippage of
the lower and upper layers. In this case there will always
exist an influx of reacting products from below and from
above into the intermediate layer. Hence, the lack of
coincidence of the hydroxyl emission maximum intensity zone
with that of the most intensive ozone formation at alti-
tudes below 50 km cannot be taken as an objection against
the ozone-hydrogen hypothesis. On the other hand, the process
of mixing will inevitably result in recombination processes
taking place more effectively by means of triple collisions
at lower altitudes,and not above 100 km where there is a
maximum concentration of atomis oxygen but where the life-
time of oxygen atoms in a free state before their reuni-
fication with one another or with oxygen molecules consider-
ably exceeds several days.
Bates and Moisiewitsch /30/ advanced a number of
objections to Kraseoveky's hypothesis. They first pointed
out that the primary acts of molecular oxygen dissociation
of about 2x1011 cm 2 sec-1 in the region above 100 km
do not suffice to ensure the recorded rate of emergence of
new hydroxyl molecules,which possibly attains 1012 hydroxyl
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molecules cm -2 sec-1. The vertical mixing of the
atmosphere provides,however,in the case of Krassovsky's
mechanism, as in the case of the ozone-hydrogen one,ample
reserves to maintain hydroxyl radiation at the recorded
level. The upward movement of considerable quantities of
ozone, which dissociates there into oxygen molecules and
atoms in about an hour's time,may be sufficient for
setting up a necessary reserve of atomic oxygen above the
region of hydroxyl radiation emergence. The downward
movement of substantial quantities of atomic oxygen causes
there more intensive processes of formation of both ozone
and vibration-excited oxygen molecules than above. It is
to be regretted that no comprehensive analysis of the
influence of atmosphere mixing on the processes of oxygen
been
dissociation and recombination has.yet published at
present. Secondly, Bates and Moisiewitsch /30/ noted
that vibration-excited oxygen molecules will be rapidly
deactivated in atomic exchange reactions with oxygen atoms,
wasting the stored up energy before interacting with
hydrogen atoms. There is no doubt that this is valid
if the concentration of atomic oxygen greatly exceeds
that of atomic hydrogen. But a concentration of atomic
oxygen below 100 km in the region of springing hydroxyl
emission has never been ascertained experimentally. It was
computed theoretically only on the basis of questionable
constants some of which are given by way of illustration
in Table 1. In addition, the chemically active excited
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9.
states of ozone were not taken'at all into consideration
in this case. It is quite possible that at night the
concentration of atomic oxygen in the region of emergence
of hydroxyl emission does not exceed greatly that of atomic
hydrogen or of its compounds.' Thin problem can be solved
only by means of direct experiments.
The question regarding the nature of hydroxyl radiation
of the upper atmosphere lacks clarity not only because of the
uncertainty with regard to the values of the constants of
possible reactions. In a personal conversation Shklovsky_
drew my attention to the fact that present-day information
about atomic hydrogen of the upper atmosphere do not
corroborate certain hypotheses regarding the formation of
excited hydroxyl as a result of low concentrations of atomic
hydrogen. Friedman and his colleagues /31/ have shown that
the concentration of atomic hydrogen at altitudes over 90
to 100 km hardly exceeds 5xlO6cm 3 or 5x1012cm 2. Below,
at the altitude of homogeneous atmosphere,the concentration
of atomic hydrogen is unlikely to be greater than by the
number of times equal to the base of natural logarithms. On
the other hand, the published extremely high values of the
rate of the reaction of atomic hydrogen transformation into
perhydroxyl /11/ raises doubts regarding the possible
high concentrations of atomic hydrogen in the region of
hydroxyl emission emergence. Table 6 gives the valise of the
mean time of atomic oxagen and hydrogen existence before
their transformation into ozone and perhydroxyl during triple
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10.
collisions with oxygen molecules or a third body. Used as
example are the largest of the published coefficients of
the rates of these reactions (see Table 1). It can be seen
that as altitude decreases, the processes of ozone and
perhydroxal increase abruptly. At night, when there is no
dissociating radiation of the Sun, it is impossible to
imagine ways for a reverse process. On the one hand, this
would be in support of the ozone-hydrogen hypothesis if
there were no appreciable concentrations of atomic oxygen
in the reaction zone, in which case newly-formed excited
ozone could deactivate before a collisions with oxygen atoms,
i.e. before the emergence of a pair of vibration-excited
oxygen molecules. But, on the other hand,effective trans-
formation of atomic hydrogen into perhydroxyl does not
substantiate this hypothesis. If one is to use the value
suggested by Bates and Nicolet /1/ (^' 10-12cm3sec-1)
for the ozone-hydrogen reaction coefficient rate, and that
suggested by Krassovsky /6/
Cl--) 10-10cm3sec-1) for the
oxygen-hydrogen reaction, and assuming the concentration of
atomic hydrogen as 5x1O6cm 3, a concentration of ozone
amounting to about 2x1Ollcm 3 or 2x109 vibration-excited
oxygen molevules cm -3 would be required, respectively to
ensure a yield of 106 newly-formed hydroxyl molecules
cm 3sec-1. These values exceed what might be expected.
Possibly more acceptable would be the existence of other
constants of reaction rates or of greater concentrations of
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110
atomic hydrogen. This would allow to preserve the former
conceptions. New precise experimental data would, however,
be required for such an orientation, and these are not yet
available. Until then one cannot uphold the viewpoint accord-
ing to which the values of reaction constants should be
rejected unless they support the hypothesis in question.
If subsequently it is really confirmed that the concen-
tration of atomic hydrogen below 100 km is insufficient to
provide,in accordance with the well-known hypotheses, for the
emergence of a hydroxyl emission of the observed intensity,
new ways will have to be found to account for the emergence
of a large number of excited hydroxyl molecules. Krassovsky
/32 and 33/ has already attempted to make a preIliminary
excursion into the realm of new presumptions. Table 7 presents
a list of some possible reactions with the participation of
molecules containing hydrogen. Of particular interest is the
chain of reactions given in Table 8. Table 9 depicts the basic
regularities of such a chain. For instance, at an altitude of
some 80 km, where it may be expected that the concentration of
all the molecules and atoms will amount to about 1Oi5cm 3, of
oxygen molecules to about 2x1O14cm 3 and of oxygen atoms to
about 109cm 3, with a3 = 10-3Ocm6see- 1 and al = 10-i3cm3
sec-1, the ratio of the concentration of perhydroxyl and that
of atomic hydrogen will be of the order of 2x103. To ensure
v9 - a yield of newly-formed hydroxyl molecules of about
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106 cm -3 sec-1, the absolute concentration of perhydroxyl
will have to be of a value close to 1010cm-3. There is
nothing improbable about such a value since the total concentr-
ation of the particles i:3 as high as 1015cm 3. In this
case the concentration of atomic hydrogen will approximately
equal 5x106cm3. If atomic hydrogen is to diffuse rapidly
upwards in the still higher part of the atmosphere and'
then dissipate, there may be no greater concentration of
atomic hydrogen there under such conditions. The process
with the participation of perhydroxyl may provide for excit-
ation of hydroxyl, but not to the high vibration levels of the
basic state. Radiation from lower levels is particularly
intensive in the radiation of the night sky. This process
would not,however, be sufficient to excite higher levels.
Other ways,too, of excitation to such levels are required.
One of the possibilities lies in the fact that perhydroxyl
itself appears in an excited state and preserves it until
the reaction with atomic oxygen, thereby providing energy
for the formation of more excited hydroxyl.
Vibration-excited oxygen molecules may also provide for
an actually recorded less intensive excitation of higher
levels. Table 10 gives a list of possible reactions. The
Table also depicts the principal regularities for processes
2. For excited hydroxyl to appear in a low concentration of
hydrogen, the concentration of non-excited deactivated
hydroxyl should be great and that of vibration-excited
molecules of oxygen and of its atoms should approximate one
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13.
another. This. follows from the fact that a5 is greater
than a6 by approximately two orders since a5 corresponds
to the reaction with the participation of a vibration - excited
molecule. With such concentrations being equal, the hydroxyl
concentration will exceed that of atomic hydrogen by two
orders or so. For 106 new excited hydroxyl molecules
cm 3sec-1 to emerge,with a concentration of non-excited hydro-
xyl of the order of 108cm 3 and a4 of the order of
10-l?cm3 sec-l, a concentration of vibration-excited oxygen
molecules is required,which attains lO8cm-3. As the concentr-
ation of atomic oxygen at night below 90 to l00 km cannot be
too high because of its rapidly joining oxygen molecules (see
Tab]e 6),vibration-excited oxygen molecules can be preserved
for a long time.
The reaction of ozone with non-excited perhydroxyl
cannot provide for hydroxyl excitation above the 3 vibration
level of. the basic state. Therefore the predominating share of
hydroxyl emission in the night sky cannot be due to this
reaction. If,however, perhydroxyl is first formed in an
excited state and preserves it before it enters into a reaction
with ozone, the emergence of hydroxyl with excitation to higher
levels is possible. It should also be mentioned that as the
rate of reactions with excited products is great, the required
concentration of excited perhydroxyl may prove to be insigni-
ficant. If, however, such conditions do not exist,ozone will
be capable of effectively ensuring the recorded hydroxyl
radiation of the night sky, provided there is a high concentrat-
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14?
ion of atomic hydrogen.
Very complex changes are observed in hydroxyl radiation
of the night sky /21/. Particularly noteworthy is the variable
relative population of the various initial levels of hydroxyl
and the dissimilar rotational temperature at its bands from the
various initial levels. On the face of it,all this is in harmony
with the existence of several mechanisms of formation of excited
hydroxyl, functioning at various altitudes. The considerable
changes in the rotational temperature,up to tens of Kelvin
degrees, even during a single night testify to the fluctuation
of the altitude of hydroxyl a mergence,since, proceeding from
energy considerations, they yield to no explanation of substant-
ial changes in temperature at any fixed level of the atmosphere.
All this provides a reason in support of the vertical mixing of
the upper atmosphere as it can hardly remain unchanged for a
long time.
In all the schemes of the above-analyzed processes,
attention was given only to the reaction of ozone or of oxygen,
molecules with atoms or with unstable compounds of hydrogen. The
reactions between hydroxyl and hydroxyl, and between perhydroxyl
and perhydroxyl, as well as between hydroxyl and perhydroxyl
result in the emergence of stable compounds: water or molecular
hydrogen. Table 11 enumerates such reactions. As the coeffi-
cients of their rate at altitudes of 70 to, 100 km may be of the
order of 10-13 cm3sec-1, they will remove effectively hydrogen,
hydroxyl and perhydroxyl atoms from the reaction zone. If one
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15.
even analyzes the processes initially described by Bates
and Nicolet /1/ or later by Krassovsky /22 and 23 /, the
concentration of deactivated hydroxyl would reach 108cm 3
at the observed rate of emergence of newly-formed hydroxyl
molecules of the order of 10 12 cm-'sec-1 or of 10 6cm-3sec`1
as well as with a coefficient of the rate of reaction of
non-excited hydroxyl with atomic oxygen of the order of
l0 2cm3 sec-1 and a concentration of atomic oxygen even
of the order of 10 10cm-3. That is why the appearance of
water vapours during collisions between hydroxyl molecules
was accompanied by a removal from the reaction zone of about
2x103 a `
hydroxyl molecules cm3 sec `1 or of about 2x109
hydroxyl molecules cm 2sec-1. To restore the initial products
a considerable greater number of hard quanta would be requir-
ed than 2x109 quanta cm2sec-1 since molecular hydrogen
and water constitute but an insignificant part of the
atmosphere and are not, therefore their only absorbers.
Apart from photodissociation there may exist other processes,
which destroys hydrogen molecules and water vapours into
hydrogen atoms or into simpler compounds. Table 12 presents
a number of such reactions. Vibrationally excited oxygen
molecules may be the effective reducer of the initial
products. Even a slight concentration of such molecules,which
would be insufficient to provide completely for a hydroxyl
emission, is ample enough to maintain the required concentr-
ations of either hydrogen, or hydroxyl or periiydroxyl in the
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16.
zone where-this emission emerges. Bates and NNiicolet /35/
assumed that the formation of atomic hydrogen may be partly
effected owing to the destruction of methane. It should,
however, be noted that although they pointed to the way of
effective destruction of methane in the upper atmosphere, it
is so far impossible to imagine any processes there,leading
to its reverse synthesis. For this reason preference has
been given in this work to the destruction and synthesis of
hydrogen molecules and of water.
.The absence of exact values of the above-mentioned
reaction rate constants, as well as the lack of reliable
information regarding the content of atomic oxygen,ozone,
vibrationally excited oxygen molecules, atomic hydrogen,
hydroxyl and perhydroxyl in the region of hydroxyl emission
emergence does not permit to analyze in detail either the
basic process of recombining atomic oxygen or its ramifi-
cations. Krassovsky /6,15 and 34/ has assumed that
vibrationally excited oxygen molecules provide for reactions
in which emissions of the night sky emerge. Along with
vibrationally excited oxygen molecules, oxygen molecules
with electronic excitation may also partly appear, as a
result of which certain emissions of the night sky will
appear, belonging to molecular oxygen.
Apparently it has now been widely recognized that at
altitudes ra;iging from 100 to 400 km,' molecular nitrogen
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17.
dissociates,in the main, as a result of ionization processes
enumerated in Table 13. A dissociative recombination of the
molecular ion is their final stage. The coefficient of
recombination is most likely assessed by values of the order
of 10-7 a 10-9cm3sec-1, depending on the nature of the mole-
cular ion /5%. It is even possible that ionization of
atomic oxygen is attended with dissociation of molecular
nitrogen as reaction 3b is more effective than direct
recombination of an atomic oxygen ion with an electrone
(see expression A in Table 13). As the concentration of
molecular nitrogen in the above region always exceeds that of
electrons, and aiO is approximately equal to 10-12cm3sec-1,
this condition is valid with a8 of the order of 10-12cm3
sec- Besides, some electrons formed during primary photo-
ionization may possess energy sufficient for ionization of
one more atom or molecule. Atomic nitrogen does not appear
to be the predominant component at altitudes from 100 to 400
km, and reaction 2 is less important than 1, 3a, 4a and 4b.
All this leads to the assumption that every act of ionization
in the upper atmosphere,whether of a nitrogen molecule or
of an oxygen atom, is accompanied approximately by disso-
ciation of one nitrogen molecule.
It has been established at present that short-wave
radiation of the Sun with a length wave less or equal to
30OX, absorbed aboce the 150-kilometre level, is the most
powerful source of ionization in the upper atmosphere /3b/.
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The total. flux of quanta of this radiation may attain
3x1010 quanta cm 2sec- 1. Above 150 km,processes 1 and 2,
given in Table 14, are incapable of ensuring an equally
effective recombination of atomic nitrogen,which could
compensate the above rate of molecular nitrogen dissociation.
Process 3 (see Table 14) whose principal regularities are
given at the bottom of the Table would most likely be more
effective. It is worth noting that a12 may be greater
than all since vibrationally excited molecules of nitrogen
oxide, formed in the reaction 3a between non-excited
products,may interact in reaction 3b. Harteck and Kopech
/37/ give for a12 a value as high as 10-12 cM3sec_l and
this has been confirmed by rocket experiments with nitrogen
oxide in the upper atmosphere,carried out by Pressman,
Aschenbrandt, Jursa and Zelikoff /38/. Hence,the concentr-
ation of nitrogen oxide molecules will be lower than that of
molecular oxygen. With v14 approximately equal to 104 of
the newly-formed nitrogen molecules cm-3sec-1, the concentr-
ation of molecular oxygen approximately equal to 109cm 3
and a11= 10-13 t 10-14cm3sec-l, the required value of
atomic nitrogen concentration will be of the order of
108 109 cm 3. It does not seem to be improbable.
As early as 1951, Krassovsky /39/ made it public that
reaction 1 referred to in Table 15 can provide for the
recorded continuum of night sky radiation. The principal
regularities of the process are given at the bottom of the
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19?
Table. For ac Kaufman gives a value attaining 10-17cm3
sec-1 /9/? As has been ascertained at present, the major
part of the continuum arises below the 150-kilometre level
/25/. An agreement with this requires that vc should not
exceed 102 quanta cm 3sec-1. This means that,for
example,with a concentration of oxygen atoms of the order
of 1010 cm 3, the concentration of nitrogen oxide should be
less than 109cm 3 and, consequently, less than the maximum
concentration of molecular oxygen above 150 km. Such a
conclusion has already been made above, but for other
considerations.
Besides the above-described process of atomic
nitrogen recombination,' two other,less effective,processes
are possible. They are shown in Table 16. Process 1, where
oxygen molecule ions are the catalyst, is possible above
the 150-kilometre level.Process 2 may occur in the region
where vibrationally - excited oxygen molecules exist,below
the 100-kilometre level, where atomic nitrogen may be
brought in as a result of vertical mixing of the atmosphere.
Krassovsky has assumed that the reaction of vibrationally
excited oxygen molecules with atomic nitrogen as well as
with carbon oxide may be accompanied by excitation of
atomic oxygen to a state 1S which is initial for the
radiation of a certain green emission of the night sky
/ 15 and 34/. Since the energy of dissociation of molecular
nitrogen and of nitrogen dioxide into a monoxide is greater
than-that of molecular oxygen dissociation, additional energy
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is released in such reactions,which is necessary for
exciting state 1S in oxygen atoms. Ozone is likewise
capable of oxidizing the atomic nitrogen penetrating
downward. Since in all the above cases a vibrationally
excited nitrogen oxide molecule emerges, basically in the
state 21 a discovery of rotational-vibrational bands
of this molecule. in the infrared region of the spectrum is
not precluded.
.The question of localization of the atomic nitrogen
recombination region is extremely important in clarifying
the nature of expansion of the upper atmosphere in daytime.
As is well known, this was noticed when observing the
braking of artificial satellites /40,41,42 and 29/. For
this process to be explained by heating of the atmosphere
with a hard electromagnetic radiation of the Sun with a
length wave less or equal to 300, the region. of the
basic recombination of atomic nitrogen,in which the trans-
formation of dissociation energy into heat takes place,
should not be very remote from the region on the atmosphere
where the above radiation is absorbed. In addition, the
acts of recombination should not substantially lag behind
those of dissociating radiation absorption. To avoid contra-
dictions with the actually occuring retardation, the latter
should not be assumed to exceed approximately 5x103 sec.
Hence, the average lifetime of atmospheric nitrogen should
not,either, exceed this valme, provided the heating and
expansion of the atmosphere in the region near the
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21.
200-kilometre level are due to the absorption of the Sun's
ultra-violet radiation with a length wave less or equal to
300A. The average lifetime of atomic nitrogen, limited
by its reaction with oxygen molecules (see process 3 in
Table 14), will equal the reciprocal of the product of the
molecular oxygen, concentration and all, the coefficient
of the reaction '3a rate.. If all is of the order of
10-13cm3sec-1, the concentration of molecular oxygen should
be of the order of 2x1O9cm-3. Such a concentration is
quite probable at a level somewhat below 200 km.
It is generally believed that atomic exchange react-
ions with the participation of atom or molecule ions are
highly effective /43/. The coefficient of their rate is
sometimes even appraised by a value exceeding 10-10cm3sec-1
/44/. If one also bears in mind that the reacting products
may possess excitation ene rgy,for instance, in the shape
of vibrational excitation of molecules,it appears ten that
the possible variants of transformations are very numerous.,
Table 17 gives a list of some ion-exchange reactions,
specifying their energy release. With the exact valies of
the coefficients of the rates of such reactions lacking,
it is not possible, howeve r,to.indicate the most probable
ways of transformations.
It is possible at present to determine more or less
accurately the yield of primary ions. But already when
evaluating their equilibrium concentration, uncertainties
appear, resulting from the lack of exact values of ion
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22.
recombination coefficients,especially during the dissociative
recombination of molecular ions. But th e most important
uncertainties lie in the insufficient knowledge of the
ion-exchange reaction coefficients.
Even before rocket investigations of the ion composit-
ion, Krassovsky /45/,proceeding from the above considerations,
assumed that the ion of nitrogen oxide,formed in reaction
3b (see Table 13), must predominate in the upper atmosphere.
Later, when it has been established by means of direct sounding
that the ion of nitrogen oxide actually prevails at altitudes
from 100 to 250 km, Bates and Hicolet /47/ raised objections
to Krassovsky's suggestion. They noted that if reaction 3b
/see Table 13/ has a rate coefficient of about 10-9cm3sec-1
(Krassovsky himself assumed the value of 10-10cm3sec-1 as a
rough estimate), all the ions of atomic oxygen will disappear
very rapidly at night, being transformed into nitrogen oxide
ions. As this has not,however,been observed, Bates and Hicolet
believe that the coefficient of reaction 3b-a8 rate has _a
value not exceeding 10-13cm3sec-1. This reaction cannot
therefore play any major part in dissociation of molecular
nitrogen. They consider more likely the formation of nitrogen
molecules as a result of the process of dissociative recombin-
ation of the molecular nitrogen ion.
Although on the face of it Bates' and Nicolet's
arguments appear convincing,still their unconditional accept-
ance calls for a full guaranty that reaction 1 (see Table 18)
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23.
has no inverse course. The point is that nitrogen oxide ions
are bound to be formed in a vibrationally excited state. If
with all that they are capable of preserving their vibration-?
al state for a long time and are in a medium with a high
concentration of atomic nitrogen, a reverse reaction appears
inevitable. In this case atomic oxygen ions will regenerate
owing to the vibrationally excited molecules of nitrogen
oxide. Hence process 3b (see Table 13) may prove to be
effective and follow its course at a very great coefficient
of direct reaction rate a8, exceeding 1010cm3sec-1, without
resulting in a rapid and complete disappearance of oxygen
ions. No data seem to be available as yet,which would
permit to reject fully such arguments without any hesitation.
Ionization through radiation, with a length wave less
or equal to 3001, related to the number of atoms of the
given element, is the same, regardless of the fact whether
they are in a molecular or in a free state. The effective
section of ionization in oxygen is somewhat larger than in
nitrogen /46/. Above 150 km, the number of oxygen atoms is
not smaller than that of nitrogen atoms. For this reason
oxygen ionization in the upper atmosphere,where its relative
content is high,cannot be a minor process. If, notwithstand-
ing Bates' and Nicolet's remarks, the reaction of molecul-
ar nitrogen destruction by oxygen ions may be considerable,
the process should be sufficiently rapid to destroy molecular
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24?
nitrogen without any appreciable retardation and to make
for heating the upper atmosphere during a recombination of
its atoms which then sets in rapidly. The maximum admissible
retardation has already been roughly estimated as
5xlO3sec. A complete destruction of molecular nitogen in
such a presumed process will culminate in a dissociative
recombination of the nitrogen oxide ion. The time constant
of this process will equal the reciprocal of the electron
concentration product and the coefficient of nitrogen oxide
ion dissociation recombination rate, and this reciprocal
will not apparently exceed the admissible value of 5x103
sec.
In recent years the Institute of Physics of the
Atmosphere under the USSR Academy of Sciences /33/ has
succeeded in discovering a regular twilight emission of
helium with a length wave equal to 10,830X, corresponding
to the transition of helium 23P -4 23S. During aurorae
lit up by the Sun, the intensity of this emission is on?a
considerable increase. Even in ordinary twilight not
accompanied by aurorae, its intensity is as high as 103
Rayleighs. N.N.Shefov /48 and 49/ ecplained this emission
as fluorescence of a metastable state of orthohelium 23S
in solar radiation. It may appear during a bombardment of
ordinary parahelium by electrons with an energy of about
25 ev. These electrons may be the product of ionization of
atmospheric atoms and molecules by the Sun's radiation with
a length wave less or equal to 300th or by electrons with an
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25.
energy of several thousand . ev, which cause aurorae. Apart
from this,ordinary parahelium,when absorbing Sun radiation
with a length wave equal to 584 A may be transferred to
the resonance level 21P and then, as a result of a cascade
transition, may pass on to the metastable level of parahelium
215. Furthermore, such metastable atoms of parahelium,when
colliding with thermal electrons of the upper atmosphere,
readily change into a metastable state of orthodelium 23S.
Before deactivation such metastable atoms may exist up to
1O3sec. Shefov has shown that to produce an ordinary twi-
light burst helium emission with a length wave equal to
10,830 R at an altitude of about 1000 km, a concentration of
atoms of orthohelium in the state 23S of the order of
10 cm-3 , formed when parahelium concentrating about 106cm,
is required. This corresponds to the density of the upper
atmosphere at this level,obtained by evaluating the braking
of American altitude artificial Earth satellites /50/.Thus
it becomes evident that already at such an altitude helium
is a substantial component of the Earth's atmosphere. The,
details can be found in Shefov's original works. This has
been mentioned here to draw attention to?a search of other
metastable states of atoms and molecules in the upper
atmosphere,which,being optically inactive,may bring about
diverse chemical conversions whose genuine nature may not
even be surmised.
All the numerical examples cited above do not mean that
they are precisely the most probable ones.. They are but
intended to illustrate what may happen to the ideas regarding
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26.
chemical conversions in the upper atmosphere if some or other
still uncertain constant will prove valid.All this will stimulate
a wide and profound discussion. It is quite evident that specie
fied or rater reliable, non-contradictory values of constants
possible in the upper atmosphere are required. What is also
needed is to ascertain the absolute and relative probabilities
or. all the transitions of such an important molecule as
hydroxyl, and this should be done not only theoretically, but
in a reliably experimental way in laboratories. This will allow
to compile an exact energy balance of the upper atmosphere,
related to the oxygen dissociation energy. It will prove possible
owing to the likelihood of fixing the true value of newly-formed
hydroxyl molecule yield by the intensity of the hydroxyl
emission in the visible and near infrared region of the spectrum,
accessible to observations. A thorough study of the processes of
formation and deactivation of metastable states of atoms and
molecules is highly necessary. Of considerable importance are
comprehensive investigations of all the emissions of the upper
atmosphere so as to pain a more profound knowledge of its
complex chemical procesces..Of enormous significance would be
complex studies directly in the upper atmosphere at ito various
levels, in different latitudes, at various hours of day and
night, and at different seasons and time periods of solar
activity cycles. It is necessary to determine simultaneously
the concentration of oxygen and nitrogen molecules and atoms,of
hydroxyl, perhydroxyl and water molecules, of atomic and molecul-
ar hydrogen,of nitrogen oxide and dioxide,of carbon dioxide
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27.
and monoxide molecules, of vibrationally excited molecules
and of all kinds of ions. This is a very difficult task.
Perhaps it is even impossible now to point to the actual
way of recolving it. But all this ' is indispensable to
eliminate the great number of uncertainties and to gain a
clear idea of chemical conversions in the upper atmosphere.
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Bates,Nicolet /I/
Krassovsky /6,7/
Kondrat'ev /8/
2)
Kaufman /9/
Hoare,Walsh /II/
Farkas, Sachsse /12/
Benson,Axworthy /13/
Table I
The rate coefficient of the reaction
6
cm sec
0+0+M--'~02+MI) 0402+M ->03+M H+02 +M -I-H02sMI
(M is 02) (M is 02) (M is 02)
-10-32
,---/10-32
10-33
'--'10-34 -10-35
-I.5 xl0- 32
10-32
10-33
2x10-34
O.IIpI.5x10-32
10-30
10-30
~- 2x10- 34
I) Here and below M denotes any atmospheric atom and molecule.
2) According to /10/ the rate coefficient of the reaction
0 + 0 + M --,> 02 4 M is also small.
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Table 2
Mainly_bel2w__50_km
2. 0 2 + by (The Runge-Schumann bands 1925-1760 02
2. 02+02 --~ 03+0
3. 03+ by (The Hartley bands 3000-2000 A) -* 02 + 0
Mainly_higher_100_km
02 + by (The Runge-Schumann continuum 1760-1250 A)--~
--'VO(1P ) + 0 (1D)
I) Here and below an asterisk (-*) denote the excitation
of atom or molecule.
Table 3
02+O+M 03+M
03+0 -~- 02+02
03}03 -, 02+02+02
0+0+M -4- 02+M
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Table 4
03
tH --)w OHS` 402
OH*. --> OH + by
OH + 0 -> 02 + H
Table 5
The-main-reactions
0+ 02+M --'~ 03 +M
0+ o3 a o2 +o2
The reactions of the deactivation
02 + H - OHX- + 0
OH * --> OH + by
Oil + 0 -- 02 + H
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Table 6
Altitude /M/1)
km cm -3
The mean life time (sec)
according to
0
H
CIRA1961
in 0+02+M --* 03+M
in H402+M -iw HO2+M
70
2x1015
I.2x102
1.2
80
4.0 x 1014
3.Ix103
3.IxIO
90
6,5 x 1013
I.2x105
I.2x103
100
1012
5x106
5x104
I) Here and below the chemical symbol for an atom ar a molecule
the square brackets their concentration.
Table 7
02 (+93.8 kcal/mole) + H2 --~ OH* + OHS`
+ 75.4 kcal/motel)
02
(+93.8 kcal/mole) + OH ?-~
0H` + 02
+ 93.8 kcal/moleI)
02
(+93.8 kcal/mole) + HO2--* OHS + 03
+ 39.8 kcal/motel)
0
+ 110
+02
OH'k+ 0
6 kcal/mole
+ 30
3
2 _
2
.
0
+ HO 2 -~- OHS + 02
+ 54.0 kcal/mole
1) 02 ( > + 93.8 kcal/mole) + 02 -~ 0 + 03
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0+HO2 --} OH" 402 (aI)
I)
OH- -~ OH+hv
0 + OH ---> 02 + H (a2 )
H+02+M --~ HO2+ M
a3)
I )a1 , a2 I and a3
these reactions.
I)
I)
are the rate coefficients of
Table 9
[0] [HO2] a1 [0] [OH] a2 [H] CO2TLM] a3 V9
v
I)
[Hi -2---- [OH] , ---9CH02_ -v2-----
r021IMIa3 a2 101 aI
EHO21 [02] [M] a,,
I) V9 is the amount of new OH-* cm-3 sec-I
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Table 10
19 02
4 . H2 - OH
4 OH
's
I)
2)
2a. 02
4 OH -~- OH
+ 02
(a4)
*
2)
2b. 02
* H -~ OH
+ 0
(a5)
2q. OH*
--~ OH
+ by
2)
2d. OH
+ 0 -~-- 02
+ H
(a6
.3 )
[02 ] [OH] a4
+ [02~ [H]
a5
vlO
[o][H] a5 = [0J ?OH] a6
1291 ' t?2 7 -- a. ----
[H] [0] a6
when
COHJ a4? [H] a5
[OH] ~r - v10
021 a4
I) -112a" is the atom exchange reaction.
2) a4, a5 and a6 are the rate koefficients of
these reactions.
3 ) ' v1O is the amount of new OH * cm 3 sec-I.
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Table II
OH+H -0+
H2
4 2.2 kcal/mole
HO2+ HO2--> 02+02
+ H2
+ 9.2 kcal/mole
OH+ OH-a- 0tH20 + 16.8 kcal/mole
0
*
O
H
0
8 kcal/mole
+ 70
9
OH+H
.
2+
2
.
OH+ 0 3
--3- HO2
+ 39.8 kcal/mole
H + 03
-3 Ii02$ 0
+ 23.6 kcal/mole
Table 12
OH
4 kcal/mole)
- 18
( H2
+ 02 )
OH +
.
H2
+ 02 -->
OH + OH
( H2O + 02 -->- H024 OH
-'70.8 kcal/mole)
+ 0
H0
O + 0
H
2
2
2
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Table 13
Ia. N2 + by
2. N2 + by
3a. 0 + by
3b. 0+t N2 -->
4a.
N2 4 e (>16 ev)
N + N+
0++ e (> 16 ev)
NO++ N (a8) 1)
0+e. (> 13 ev) ---)w 0++ e 4 e
A. [ N2} a8 >> [e ] a10
Ib.N2++ e ---~N+N (a 7 ) I)
3c. NO+te ,N+O (a9) 1)
4b. N2+e(> 16 ev)-~--N2+fe+e
I) a7, a8 and a9 are the rate coefficients of these
reactions.
2) a10 in the coefficient of the recombinations of 0+
and electron into 0.
Table 14
I. N + N + M --- N2 4 M
2a. N+O+M -~ NO + M 2b. 140+N ?-b N2 4 0
3a. N + 0 NO * + 0(a1I)1) 3b.N0* t N--"-N2 +O(a2 12)I)
[021 [N] aII
[NO]][N] a12 N v14 2)
[NO J c aII [ 021
a12
[N] -' -v14---
NELI I
I) a11 and a12 are the rate coefficients of these reactions.
2) v14 is the amount of recombinations of N and N into
N2 cm-3 see-'
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
I.
No 4
0--'1102 + by (ac) 2.N02 0 --3 N0 + 02
[NO] [ 0] ac = vc 2)
I)
ac is the rate coefficient of this reaction.
2)
vc is the amount of quanta of the continuum
cm-3 sec-I.
Table 16
Ia.
02++ N --> NO+* + 0
(4 4.11 ev)
lb.
NO" + N --~- N2 + 0*
(- 0-83 e v )
Tic.
0+ 4 02 --s. 0 2+ + 0
(4 1.40 e v )
2a.
02 + N -~ N0 ` 4 0
*
-
*
2b.
- NO 4 M
NO
+ M
#'
2c.-
NO + N N2 + 0
2d.
NO + N -* N2 + 0
Table 15
I
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Table 17
Reactions
Energy
ev
+
+
N
NO
0
8
02
+ N2
O
+
.
4
N2+t 02
--~
NO+ + NO
+ 4.29
02++ 0
-->
02 + 0+
- 1.40
02++ N
--~
NO++ 0
+ 4?II
0
+
N
0+ + NO
+ 0
01
2
+
.
N24+ N
--a
N2 + Nt
+ I.II
0
N
+
--
NO++ N
+ 2
88
+
2
~
.
0
4
N+ + NO
16
- 2
N2
+
.
+
+
4 0
NO
02
+ N
- 4?II
+
0
+
6
+ 0
NO
+
2
N
-
.45
NO++0
NO+0+
10
- 4
.
+
--
0
+
2
88
N0
+ N
~
N2
+
.
NO++ N
-~
O++ N2
0.83
NO+++ N
NO 4 N+
5
04
.
0+ 02
0 + 02
I.4O
0+
N
>
NO+4 N
+ 0
8
+
2
.
3
O++ N
-- >
N+ 4 NO
4
21
2
.
N4`
N
N
+
N
- I
II
+
2
>
2
t
.
N4+ 0
NOtt 0
+ 6
45
2
.
N t 0
--
0++ NO
0
67
2
~
.
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
Tab le 18
0# t N 2 N 0+ # N
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246A016600420001-1
It D.R.Bates and M.Nicolet. Journ.Geophys. Res. , N 3,
301, 1950
2. D.R.Bates. The earth as a planet. Ed.G.P.Kuiper, p. 576,
1954-
3- P.Harteck, The threshold of space. Ed.Ivl.Zelikoff, p.32,
1957.
4. M.Nicolet. The threshold of space.Ed.M.Zelikoff, P-40,1957-
5. A.Dalgarno. Ain.G6ophys. 17, N I, 3.6, 1961.
6. V.I.Krassovsky. Usp.Fizich.Nauk, USSR, , N 4, 673P1957-
7. V.I.Krassovsky. Journ.Atm.Terr.Phys. 10, 49, 1957-
8. V.N.Kondrat'ev.Kinetics of chemical gaseous reactions.
Publ.Iiouse Academy of Sciences,Moscow,p.283,1958.'
9. F.Kaufman.Proc.Roy.Soc. 247A, N 1248,123,1958?
10. W.D.McGrath and R.G.W.Norrish. Proc.Roy.Soc.,242A,
N 1230t26591957-
11. D.E.Hoare and A.D.Walsh, Trans.Faraday Soc., 1102,1957.
12. L.Farkas and II.Sachsse. Z.phys.Chem. B27, III, 1934.
13. S.W.Benson and A.E. Axworthy. J.Chem.Phys. 26, 1718,1957.
14. G.Herzberg. J.Roy.Ast.Canada 15, 100t1951-
15- V.I.Krassovsky.Usp.Fizich.Nauk,U.S.S-K., 47, N 4,493,1952;
54, 11 3, 469,1954.
16. J. D. IvMclinley , D. Garvin, lvl. J. Boudart . The airglow and the
aurorae.Jd.E.B.Armstrong and A.Dalgarno.
Pergarnon Press,London. p. 264, 1955?
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
17. N.N.Shefov.Spectral, Blectrophotometrical,and Radar
Researches of aurorae and Airglow. Publ.House Academy
of Sciences,Moscow,N 6, p.21, 1961.
18. D.Garvin, H.P.Broida and H.J.Kostkowsky. J.Chem.Phys.
32, N 3, 880, 1960.
19. I.S.Shklovsky.Izv.Krym.Astrofiz.Obs. 7, 34v1951-
20. H.S.Heaps and G.Herzberg. Z.Phys. 11339 48, 1952.
21. V.I.Krassovsky, N.N.Shefov and V.I. Garin. Journ.Atm.
Terr.Phys. 21, 46,1961.
22. V.I.Krassovsky and V.T.Lukashenya.Doklady Acad. Nauk USSR
81, 811, 1951-
23. V.I.Krassovsky. The airglow and the aurorae-Ed. E.B.Arm-
strong and A.Dalgarno. Pergamon Press,London,
p.193, 1955
24. R.G.W.Norrish,etc. Proc.Roy.Soc. A.233, 455,1956.
25. D.M.Parker. Ann.Geophys. 17, N 1, 67,1961.
26. T.M.Tarasova ? Astr.Zirc. U.S.S.R., N 222, 31,1961.
27. V.I.Krassovsky. The airglow and the aurorae. Bd.E.B.Arm-
strong and A.Dalgarno. Pergamon Press,London.
P-197,1955-
28. M.Nikolet. The earth as a planet.1d.G.P.Kuiper. Pp. 644,1954
29. M.Nikolet,Physics of the upper atmosphere. Ed.J.A.Ratcliffe.
P.17.1960.
30. D.R.Bates and B.L.Moiseiwith.Journ.Atm.Terr.Phys? 8,
305,1956.
31. 11-Friedman. Proc. 11 Intern.:~stronaut.Congress,Stockholm.
P.83,1960.
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
32. V.I.Krassovsky, Usp.Pizich.Nauk,U.S.S.R. 75p N 3,501,1961.
33. V.I.Krassovsky.Plynet.Space Sci. 8, 197,1961.
34. V.I.Kras6ovsky.Ann.Geophys.14,N 4, 395P1958-
35. D.R.Bates and M.Nicolet.Pub.Astr.Soc.Pacific 62,106,1950.
36. H.F.Hinteregger.Journ.Geophys.Res. 66, N 8, 2367,1961.
37? P.Harteck, V.Kopsch. Z.Phys.Chem. 12L32791931-
38- J.Pressman, L.M.Aschenbrand, F.F.Marmo, A.S.Jursa and
M.Zelikoff.The threshold of space.Fd.M.Zelikoff.
P-235-1957-
39- V.I.Krassovsky.Doklady Akad.Nauk U.S.S.R. 78 , 669,1951-
40- M.L.Lidov, Isk.Sput.Zemli. Publ.Hause Academy of Sciences
U.S.S.R.,Moscow. N 1, 9, 1958.
41. P.R.E1'yasberg and V.D.Jastrebov.Isk.Sput. Zemli. Pubi.
House Academy of Sciences U.S.S.R.,Moscow.
N 4, 18, 1960.
42. G.A.Kollegov.Isk.Sput.Zemli.Publ.House Academy of Sciences
-U.S.S.R.,Moscow.N 4,31, 1960.
43. H.Eyring, J.0.Hirschfelder and H.S.Taylor.J.Che m.Phys.
4, 479, 1936.
44. R.F.Potter, J.Chern.Phys.23, 2462,1955.
45. V.I.Krassovsky.Izv.Ac.Sci.U.S.S.R.,ser.geophys.,N 4,5.04,19570
46. A.Dalgarno and Parkinson,Journ.Atrn.Terr.Phys. 18, N 4,1960.
47. D.R. Bates and Nicolet.Journ.Atm.Terr.Phys. 18, 65,1960.
48. N.N.Shefov.Planet.Space Sci.5, 70,1961.
49. N.N.Shefov. Ann.Geophys.17,N 4,1961.
50. H.K.Paetzold and H.Zschorner.Pr?oc.2 Cospar Symposium,
Flovence,1961.
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/30
6/ A.D.DLNILOV
iv .
'1SOME QUESTIONS, CONNECTED WITH RECOMBINATION AND
IONIZATION PROCESSES IN THE EARTH ATMOSPHERE"
I. The knowledge of the value of the effective recombination
i
coefficient in ionosphere is of great importance for
understanding a number of questions of upper atmosphere physics.
The analysis of various photochemical reactions, controling
upper atmosphere ionic composition, made in works (1,2,31
allows to investigate diurnal variation of Ott
value at
different altitudes.
At present it is common knowledge that molecular ions
dissociative recombination reactions are the basic recombination
processes in the upper atmosphere. Work (4J shows, that at
least up to the 500-600 km altitudes recombination in the
atmosphere is defined by the reactions:
NOt?e N#O
-t e- 0+0
14++e. ~N+N
and effective recombination coefficient is written in the
following form: +,
cL! oC L X
~
,-
where d - rate coefficient of dissociative recombination
t
reactions, Xv1 - summary concentration of molecular ions
at the given altitude.
As up till now the exact oL coefficient value remains
questionable, one can consider diurnal variations of a(! value
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without assuming a fixed value for this coefficient. As is seen
from /I/ of value is proportional to molecular ions part in the
total ion density rX"]Ins / ne /,therefore, the
question of o(, value dirunal vai'iation comes to the investigat-
ion of diurnal variations of molecular ions quantity in the
atmosphere.
At present there are no reliable experimental data of
atmosphere ion composition variation from day to night.
V.G.Istominn measurements [5,67 taken during morning and evening
hours of different days, allow to make only qualitative
conclusions. The same can be said about the measurements by
Johnson et all !'TI, taken in more nothern latitudes, than
V.G.Istomin's measurements, what makes difficult their mutual
comparison.
Works [1-31 deal with photochemical ways of molecular
ions formation and there were obtained the following
expressions for concentrations ratio
LNotj [N?] t?i J .., [ol [l-rs 1 - [N:
(0 3 Me , Lo?] Me (o+7 ne
which turned to be in good correlation with the mentioned
experimental data. As can be seen from these expressions, the
ratio of molecular ions concentration to the concentration of
atomic ions is directly proportional tb neutral density and
inversely proportional to electron concentration.
if
-
In view of the said we transform the ratio " 1, in
e
formulae /I/ as follows:
CxA 1 +- [XN ] C__T /2/
C xN J t +1 + LXM J- + fNo`J+(o21 t(ti 1
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As, according to experimental data (81 /N+J at all-the
altitudes does not prevail 1/10 of fO+J, the second term in
the fraction numerator can be neglected. As to this fraction
denominator, the part of 02 and N2 ions relative to NO+ ions
varies from 1/5 -1/10 at low altitudes to 1/2 - I at the
altitudes of the order of 500 km therefore, assuming an
error, fully aware that it is within the factor of two, one
can substitute the value 195 [NO+J for the fraction denominator.
Then formulae /2/ will have the form:
Cx''1 4- 0. (OS _
W01
According to '(IJ ?7 : Y,? C= , where - the
ratio of the rate coefficients of charge transfer and dissociat-
ive recombination reactions, which was found in the given work
to be equal to IO-4. Thus, the resulting formulae for effective
recombination coefficient will have the form:
I = d'
nc /3/
*v -
1 4- o,bc?lo? CNA 1
This formulae allows to consider od value variation
from day to night on the basis of diurnal variations of
Neutral and electron densities at various heights. Diurnal
variations of atmosphere density is taken from the work by
King-Hile (9J, and day to night electron concentrations ratio
is taken according to Ja.L.Alpert (IOj. Up to the altitudes of
the order of 200 km the value /0y
in formulae /3/
Mil
is small in relation to 11 a
/what corresponds tolsmall part of
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atomic ions relative to molecular ones/ and oL' practically
does not vary from day to night. From 200 km to 400 km the
ratio -(~d~~) ~ day is inversely proportional to the relative
nigfi~
electron concentrations ratio. Above 400 km diurnal variations
both electron and neutral densities must be taken into
consideration. Assumed values ~ he) n day g and (p) nag
and the obtained ratios rte'/ night for the 100-600 km
altitudes are listed in the following table:
H km
100-150
160
180
200
250
300
350
400
500
600
(ne) da
10
20
20
20'
20
18
8
3
2.7
2.7
he) nigh:E
d
I
I
I
I
I
I
I
1,5
3.8
8.0
(,P )
Night
night
I
1.1
1.3
1.6
4.6
10
6.8
2
0.8
0.34
day
As can be seen from the table, effective recombination
coefficient up to the altitudes of the order of 400 km is highe;I
than in the day time, the greatest ?cr variations occuring at
about the 300 km altitude, reaching an order of the value.
Above 500 km effective recombination coefficient has inverse
diurnal variation, i.e, decreases at night.
On the basis of the above said it will be not difficult to
estimate diurnal variation of the total number of recombinations
c According to the table
in an atmosphere colupn f at n
data the ratio (1 al na d / day/ (Jc.lhez)niht has the
value 3.3 101?
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2. Experimental data of ion and electron concentration in
the ionosphere allow to consider the question of ionizing agent
absorption in the upper atmosphere.
As is show in [4l the total rate of recombination in a
volume unit jar la second at the given altitude is equal to:
Y, e et = Ot [xAlm'1 t7 e- /4/,
where all the designations are the same as at the beginning of
the paper. In equillibrium conditions the recombination rate
must be baikiced by the ionisation rate:
Y,~ =Y'oN - CM72~ n = [141i 15/
where C M 1 - neutral particles concentration in a volume unit,
T dj - ionisation cross-section, n - ionising agent flux
at the given altitude, j - ionisation coefficient. The last
equality is true only for monochormatic radiation or for the
radiation , the cross section of which does not vary with Wave
length.
Radiation flux value must vary with height and depend upon
optical depth of the above atmosphere layers:
Z cell
n = h ? e . n~ e
where he - ionising agent flmx outside the atmosphere, Z -
optical depth, NM - the number of particles in an atmosphere
column above the ;iv&n level. Denoting 2;h,p by
d
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/ionization coeffecient Outside the atmosphere/ we write tho
last equality;
/6/.
As is clear from this equality, value variation with height
under the given atmoophef'e density is determined by absorption
cross-section . On the other hand, from equalities /5/ and
/4/ one can obtain the following expression for
the given altitude:
? rX+7ti
[M 1
Fig.I shows the values for the altitude range 100-400 km
/point/calculated from formulae /7/. While calculating there
were used experimental data of electron /II} and ion (8,6J
densities. The value (IAI is calculated on the basis of the
density experimental data (12,I3) in supposition, that the par
part of molecular nitrogen up to the 400 km altitude remains
constant (14J, but 02 and 0 concentrations are distributed in
accordance with (2J.
Fig.I shows as well an absorption exponential curve /6/
in the altitude range 160-400 km, when e value is ecual to
5 ? IO-I7 cm2. As is seen from this figure the ionization
coefficient variation with height at the altitudes above 160 km
is well represented by the absorption curve, corresponding to '.
high aborption cross section 5 I0-17 cm2. At the same
time, one can see from Fig.2, where ,( - value variation with
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height below 160 km is shown in another scale along the altitude
axis, that at low altitudes i - value variation cannot be xapraail
represented by exponential curve, corresponding to any single
absorption cross section for the whole altitude range 100-160 km.
As can be seen from the curves of Fig.2 the cross section,
corresponding to ionizing radiation absorption at these altitudes
varies from I0-17cm2 at the 150-160 km altitude to 5 10-19cm2 At
the 100-110 km altitude.
The obtained ionization coefficient variation in the
atmosphere seems to be indicative of the following: at the 160-
400 km altitudes the ionization in the atmosphere is produced
by the agent, having high vross section of absorption by atmosphere
components.
Besides, this agent is qLonochromatio in the sence that its
absorption cross section does not vary while this agent is being
absorbed a hundred times. The mentioned characteristics lead to
s~t. L
a supposition, that l~altitudes above 160 km solar ultraviolet
radiation cannot be the ionizing agent. Indeed, firstly, the
maximum cross section of absorption by atmosphere components of
solar ultraviolet radiation is i.0 IO-I7 cm2 (151, the mean value
of 49 being equal to 3-5.I0-18 cm2 (161.' Secondly, the Solar
ultraviolet radiation is not monochromatic, i.8. it consists of
radiation "parts2, having different absorption cross section from
the given maximum value to the values of a few units per I0-19cm2,
therefore this radiation absorption at different altitudes must
correspond to different IO-8. To carry out these measure -
ments as well as to carry out them during other ionospheric
disturbances , it would be necessary to have higher rates of prc
processes and more accurate measurements. Therefore for -Ii
determination it is used n 0 relative variation during the eclilw
By this method for ,/' 0.5-2.I0-g values are obtained. However
here it is not taken into accoitut the fact that at the moment
of maximal phase about 10-20 percent of solar extreme ultra-
violet radiation coming outside the solar disc, as it was recent
ly prooved with the help of rocket experLaents. Considering
this fact a ni tuber of authors obtained
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= 0.4 - 1.10-7 /12 - 16/, though it may happen that higher
values can be obtained, especially if we take into account
that bright regions of extreme ultraviolet are distributed
over the disk nonuniformly. These c:1 r datat are in a goy 1 agree-
ment with those ones presented in Table I and are supported by
other ionosphere measurements. For example, a certain sharp
variation of ne at sunrise'and sunset also leads to an un-
usually high value of c~' and measurements of the aurora
brightness variation gave also high values of C4/ =I0-7-IO 6.
In connection with it is also necessary critically to revise
the conclusions concerning , obtaining in diurnal variation
of ne and some other methods. It. also,necessary critically to
reconsider interpretations of another phenomena co~inected with
recombination and ionization rate in the ionosphere.
On the bases of the conclusions of high rates of re -
combination ionosphere processes, the main chemical reactions
describing elementary ionosphere processes must be revised.
Bates and 1.1assy /10/ considering various possible chemical
reactions in the upper atmosphere indicated in particular disso-
ciative recombination and ion-atom interchange reactions. Other
authors paid great attention to these reactions, however only
now it was established that they are of significant importance.
Using the data concerning the variations of relative ion
composition with the height, Danilov /9/ confirmed that ion
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transformations and disappearances occur mainly in such a way
that atomic ica. transforms into molecular ones caused by. ion-
- atom interchange reactions,and neutralization in the iono-
sphere occurs as a result of dissociative recombination of
molecular ions. In this case, as it was shown by Ratcliffe /19/
electron disappearance rate in the upper part of the ionosphere
should be. proportinal to ne but not to ne , as it is in the
lower ionosphere. The linear law of electron disappearance at
250-400 km heights is obtained now in a number of experiments
and this also confirms that the choice of the abovementioned
reactions in the ionosphere was quite true. Rate values of
ion formation and ion dis4pperance at 200 - 400 km height obtair
ed eclipse data in /20/ are close to those ones presented in
Table I; Van Zandt et.al. /20/ also indicates contradiction
between those data and the existent data concerning--'/.
3) According to new d.ta concerning the recombination
coefficient the ionosphere should be neutralized for a
compdrattvely chort period of time after sunset, if there was
no edditinal night ionization source. Antonova and Ivanov -
- Kholodny /21/ suggested a corpuscular hypothesis to explain
night ionosphere ionization. According to this hypothesis a
soft (102 - I04 ev) electron flux according to -1 new data
with power of .- I erg/cm 2sec fall onto the ionosphere. This
electron flux may produce some ionization even in the day
time /21/ at 300 km height it may produce ionization exceeding
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e ole caused b; ;cola+.r extreme ultra-:.violet. his as3umption
may explain the n ted difference betweeii data concernin~
in sable I at 250 300 km height obtained in various ways
and also a peculiar variation of with height, indicated
by Janilov /9; 22/, ,.,rho ciie attention to high effective
cross section of the ionizinC agent at "300 km height. It is
imaortant to emphasize that the source power necessary for
producing e-.ectron fluxes in the ionosphere must exceed many times the
source power of the earth radiation belts. The hypothesis
concerning the soft electron presence in the. ionosphere is a
significant contribution to the development of now ionospheric
point of view, and it is closely. connected with high rate
conception of ionization and recombination processes in the
ionosphere. An experimental foundation for the corpuscular
hypothesis is presented in detail in /21/. Here it should be
added that recently Kazatschevskaya et.al. have confirmed by
new methods in experiments with thermoluminescent phosporaV
Antonova's experimental results, the latter obtained that 70-
100 km height the flux of 20-30 kev electrons carried the energy
of about I.IO-2er,-1/cm2see. steradian. Let us note that we can
directly obtain the value of the rate coefficient of the
ionization processes consequently near 100 km height gzI02cm 3
,jec -I, caused by the abovemmntioned electrons, and the rate
::acombination coefficient balancing this night ionization
-% 3.10 ~ .
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-II--
So we believe that the whole co~ le of ne,.~J rocket expe:i-ii.e.7tc.i.
data esti=.ting intensities and solar extrre:ne ultra violet spectrum
its distribution over the solar disc and beyon4 the limb, estimet-
ing ion composition and corpuscular radiation in the ionosphere
show that the oppinion concerning rates of recombination and ion-
ization processes which has been formed by the present time, is not
true. It was indicated above in what way these ideas concerning
elementary processes in the ionosphere should be reconsidered. Here
it was found out, that the conclusions delt with high intensities
of ionization and recombination procedses are also confirmed in a
number of ground ionosphere experiments. In connection with it,,
now it is probably necessary critically to recosider earlier obtc~ine
ed results of effective recombination coefficient measurements.
-Chore arises a question of developing new ideas concerning physical-
-chemical ionosphere processas as well as concernin new interpret-
ion of such phenomena as a general. ionosphere behavior and also iono
sphere parameter variations dependently on the time of day, season
geographical co-ordinates, and also on upeper atmosphere heating,
diffusion and drift.
Institute of Applied Geophy-
sics of the Academy of
Sciences of the USSR.
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I. H.L.Newell,Jr., in,"Physics of the upper atmosphere", ed by
T.A.Ratcliffe, New York - London, 1960,P.273.
2. G.S,Ivanov-Kholodny, G,Idi.Nikolsky, Astronomitch. j., 38,828,
1961., "Prediction and Identification of Em'ssior,
Lines in Solar Extreme Ultraviolet II00A"
(report presented at this symposium)
3. C.13.Aillen, Terr. Magn.Atm. Electr., 93,433,1948.
4. I.S.Chklovsky, Izv.Irym ~' sk.astrofizitch.observatorii,J,80, 1949.
I96I.
5, G. S.Ivanov-Kholodny, G. il. rlikolsky, Astronomitch, j . , 3II, 45,
6. H.Kallman-Bij1,R.2.F.Boyd, H.La Gow, S.M.Poloskov, W.Prister,
"Cospar International Reference Atmosphere", 1961
7. G.S.Ivanov-Kholodny, Geomagnetizm i Aeronomija (in press)
8. G.S.Ivanov-Kholodny, Dokl. AN SSSR, 327.1961
9. A,D,Danilov, Dokl. AN SSSR, 137,1098, 1961.
10. D. R. Bate:, H. S.N.Iuiassey, Proc, Phys. Soc., 192,1947
II. D.R.Bates, Phys.Rev., 78,492,1950.
12. O.E.H.Rydbeck, Wilhelmson,H., Trans. Chalmers Univ. Technol.
Gothenbe.'G, Sweden, N 149,3,1954.
13. I.Hunaert, tiT.Nicolet, ;.Geophys,`tes., 60,537,1955.
14.C,1M.Minni.,, Nature, I7FB,33,1956.
Atm.'-''err.l'hys.~ 9,20I, 1956.
15. C.M.A,Iinnis, J.
16. 1.A.xnteliffe, "Soler eclipses and the ionosphere", 1956,p.306.
17.14I.W.Mcelhinny, J.Atm.Terr.Phys.,14,273,1959.
13. T.A.Chubb, H.Friedman, R.W.Krnplin, R,1$1xBBl1ke6, A.E.Ungicker,
MA-M. Soc. roy. 5ci. , LiLoe, 4 ,22,
,IAtin. '2err. Phys. , 8, 260,I956.
19. S.A. Ratcliffe,
20. T.E.Van Zand, R,B.NNorton961C.H.Stonehocker, J.Geophys.Res., 65,
2003,
21.Liri.\ntonova, G.S.fvanov-Khohlodny, 'Geomagnetizm i aeronomiya",I;
"164, 1961 "14pace Research!I" Amsterdam, 1961. r 22. A, D,Danilov " SOmonizationnprocessesein4Jtte earthbatmosphere't
(report presented at thts~symposium)
23. T,V.Kazatchevskaya (private conn,latio?Z.~ ? AN SSSR (ser.geof.)
24. L.A. Antonova, ~1?o1odny,
N 5,756, I960
25. L.A.Antonova)Izv6stiya AN SSSR (ser.geof.) N9, 1437, 1961.
26. Ya.L. Alpert, JETF, 18, 995, 1948.
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4v T. M. TARASOVA
I2 , NIdHT Slil M.AIi+ i:L(I3SION LI tJ3: INT N3ITY DISTRIBUTION WITH HEIGHT
The results of the preliminary treatment of the experimental
data obtained on the 23-d of September, 1960 are presented in
this paper.
The aim of the experiment was the investigation of the
night sky emission line energy line distribution with height it.
possible close conditions of the experiment for all the lines
(apparatus orientation, closeneau of the studied regions of the
sky and measurement momerits~. In the apparatus it is provid+:d
simultaneous (with maximal intervals 1.6 sec) measurements of
the green line glow ( .A =5577 R) and of the red line (,A =6300
atomic oxigen, sodium ()s. =5893 R), hydroxile (9.I00-I0.700 R),
molecular oxigen ( A =3650 and of the confrinuous spectrum
of the night sky ( A =5300
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I.APPA;RATUS. A photoelectrical. photometer was used, it
was raised on a rocket to high atmosphere layers. This
photometer as an automatical device, having two optical
channels with receivers, providing the apparatus. sensitivity
in the region of 2600 -!4.000 R. An illumination of the cathodes
is made by means of two telescope systems operating parallely.
Frequency of filter changing is 0.4 sec. Photometer ktdy/N~ angle
:Ls 6?. The photometer axis. is set up parallel-., to the rocket
axis. In order to control& apparatus operation stability' Zt
is mounted a luminaphor of a constant activity. The record was
carried out by means of an oscillator with 12 galvanometers
that made, it possible to record one and the same energy value
in five ranges. The time of the beginning of instrument operation
is (00h56m) of local time.
2.PROCESSING METHODS AND CALIBRATION. Calibration was carri
ed out by means of a band lamp, colour temperature of which
and its integral energetic power of light are known. Illumination
of the, objective of the system was made with the help of a
frosted glass, spectral transparency of which and its evenness
of illumination were estimated experimentally. Optical
characteristics of interferent filters were estimated by means
of a monochromator under the same illumination conditions, under
which the instrument operates, when measurements are being
carried out. Photometer calibration was carried out by meano
of experimental determination of the frosted glass brightness
with the help of a thermal element graduated in absolute energy
units, according to a standart lamp. The frosted glass brightness
obtained experimentally coinsided with the calculated value
obtained according to Plank's equation.
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Data processing was fulfilled in the followin;; way. The
apparatus reading when measuring hiht sky glow;
i,4= C
.h ('r , 6,~ + - o YW ) W J
where 6 a _ 6 , 1 J~ + dk
A
B - radiation brightness in the line
~~ - continuous radiation brightness at I
fQkU W - radiation brightness in the corresponding hydroxile
band, passing through the filter
- solid sight angle in steradians
S - objective area of the system in cm2
.- the equivalent filter width in i. for 100 per.cent. of
penetration which is equal to estimation
,~-4ve ten~~~i
K.k - filter penetration coefficient,ln#Alfinress~/eo,
C,X _ proportionality coefficient,
penetration is also taken into account.
When considering the continuous spectrum background we used:
Roach's /I/ assumption, according to which continuous
background distribution is taken as identical with the energy
distribution in a2 star spectrum class.
Another method of the background calculation with the use
of Shefov's experimental data /2/ leads to certain variation of
the absolute values of the intensities, but does not introduce
considerable changes into the relative glow intensities
distribution with height.
For the emission of OH and 02 the continuous background was
not considered at all. The accuracy of the intensity estimation
in absolute unit is 30 R,The accuracy of the relative line inienx
intensi-ty
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1g- estimations is 15-20 per cent.
The paper presents the data, obtained at the ascending
branch of the rocket trajectory from the height of H=65 km
(when the instrument starts operating) up to the height of 200km
The orientation accuracy estimations for the height range
of 65-100 km is +20, for I00-I30tm- +10? and for 130-190 km
- +20?. The apparatus movement at the ascending trajectory
branch may be described in the following way: in the region of
65-75 km the axis is directed to the zenith, beginning with
75 km height the apparatus starts turning and this is followed
by increasing of the measuring intensity value caused by the
ray path increase. At the height of 130 km the apparatus axis is
directed just vertically down, at 170-200 km height the
apparatus keeps on rotating and its axis is again directed
to-wards the zenith.
3.EXPERIMENTAL DATA are listed in Table .I and illustrated
in graphs No.I-6. In t4e first line of the Table there is fixer:er
presented the agent that causes a glow; in the second line the
inxestigated spectrum region; in the third one-filter spectral
characteristics which were obtained in view of spectral
multiplier sensitivity; in the fourth line - energy values, Kkti
which were obtained on the ground on the eve of the rocket
experiment. For OH and 02 emission there are relative
intensities I, as for the rest of the components there are
rn
absolute intensity values"Rayleigh: - summary intensity
measured by the apparatus in the given spectrum region
e of -IAa EL" p21AA the MOM
L toH is the energyYoT the corresponding hydroxile band ( the latter
is taken from literature data )
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/3/ and E., - the energy in the emission line; in the fifth line
- the same values, recorded by the photometer at the time of
passing H=65 km X directed towards the zenith (h. In the sixth
line - the data, obtained by the apparatus at 130 km height
the axis is directed vertically down (h). The data. obtained at
130 km, when the apparatus axis is directed-towards the Earth,
may be distorted by an additional light source from the Earth.
However, practical equality of OH emission erlgy ratio in the
nearest infrared spectrum region to the green line emission
observed at the heights of 65 (f) and 130 (1) indicates that
both cases we deel with the atmosphere own emission. When an
additional light source appears should sharply decrease
this ratio due to considerable difference of a spectral energy
distribution in the night sky and in an electrical lamp. In the
seventh line there are emission values, recorded by instruments
at I80 km height, when the axis is directed towards the zenith;
in the last line -,the energy difference, obtained in lines
5 and 6, that determines the glow intensity coming from the
heights exeeding 130 km.
In Hig.1-6 the apparatus climb height is plotted on the
abscisse: in all the Figures curve 3 gives the intensity record-
ed by the photometer in the position it appeared to be at the
moment of measuring(the curve is drawn according to four scales
x - in the text (t) means that the apparatus axis is directed
towards the zenith, and 0) means that i$ is directed vertical-
ly down.
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which are provided by the oscillator with galvanometer); curve I
gives the intensity reduced to the zenith, which is obtained
from curve 3 after the introduction of a correction for the zexx#
zenith distance according to the following equation:
I) for the case when the layer is above the apparatus
1 ='7 J& (, where 6/7 _ Rt
2) for the case when the apparatus is moving in the layer
'9 aple
where - the intensity when one obverves it in the zenith
direction;
- the angle of the apparatus and the vertical;
R - the earth radius
No - the ap arattus altitude.
H- X
When calculating corrections for the maximum upper boundary
of the layer for = 9100 - 10700 R , )= 8650 R , A= 5577 'dk the altitude of 120-130 km was taken; according to% our data
oWe
there is no glowVthese a titudes.
In all the Figures on curve 3 arrows show the altitude
range for which the correction or the zenith angle is less than
20 per.cent,the arrow direction is the directrion of the
apparatus axis.
Curve 2 is obtained by differentiation of curve I and it
gives emission in atmosphere volume units.
4. DISCUSSION OF THE RESULTS
)
I) Hydroxile emission (9100 - 10700
As it is seen from the Table and Fig.I the energy value,
recorded at the altitude of 65 km ( (),when recording a glow
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is the whole depth of the atmosphere above 65 km, coinsides with
the accuracy of test errors, with the energy value, obtained at
the 130 km altitude, when measuring glow in. the 0-130 km layer.
The glow energy distribution with height is given in Plot
No.I, curve I. which was obtained when the apparatus wie crossing
it. As it is seen from this Plot the glow is concentrated in
the layer the low boundary of which is at H * 73 ? 2 km, and
the upper one is at H = 110 + 10 km. The layer gravitation center
is situated at H * 78 2 km. At H= 180 km the photometer records
only continuous radiation energy and this is less than 10 per.cent
of the energy at H = 65 km. At the altitudes below 65 km there
probably exists glow in the region of 9100-I0700 k , as
J65(}) J130(') expected energy values are, however, within
the limits of the test accuracy.
2) 0?(0-1) molecular ox.gen emission.
The data for 02(0-I) presented in the Table and Fig.2 show
that in the region of A = 8650 R a glow is concentrated in the
layer, situated between the altitudes of 65 and 130 km, as energy
value, recorded at 65 km (f) is practically equal to that one
recorded at the 130 km altitude (1 ) and aJ = ((w) const at
H = 65 - 74 km. At altitudes exceeding I80 km the glow is lacking,
~~nly the continuouri>> radiation ene.rr y ie LIP-acurpL and it
ifiJ
_.~._.. - _ as it is seen mob. cVie.~.~ Lctil~~ per. cent
of the energy at H=65 km. From curiae I, Plot 2, where the vertical
emission distribution is given, it is clear that the low layer
boundary is at H=74?2 km, and the upper one is at H = 110 ~ 10 km.
The layer gravitation center is situated.
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at H== 8I+21an.
According to preliminary estimates the molecular oxygen
energy radiation value is 50 per.cent of the summary energy,
coming through the filter; 50 per.cent of the glow is induced by
the hydroitile glow and the hight sky continuous spectrum
background. As the energy value of JN = 130 (h is somewhat
higher than JN:65 (1) it is. likely that below 65 km there
exists glow in the region of -X = 8650 , however expected
energy values are in the range of experimental accuracy.
3. Night Sky Glow Continuous Spectrum
As it is seen from Plot 3 for the region of = 5300
in the height range of 64-75 km the part of the curve _ ((H)
=const, which is characteristic for the came when the layer is
above the apparatus (see Fig.I and 2) is lacking. The intensity
begins decreasing, when the apparatus starts operating and goes
on up to the altitudes exceeding 130 km. This can be seen from
the T&blw data analysis: at H=65 km the energy value computed in
R is equal to I R/R ; at the 130 km altitude this value is equal
to 0.4 R/R. Comparing these figures we can conclude that the
energy of the radiation, coming from the altitudes excedding
130 km, should be no less than 0.6 R/R. Actually the energy
value recorded at 180 km altitude gives only 0.4 R/R. This
testifies to the fact that above 130 km in the region of
fl, = 5300 R, there exists glow, which is of an atmospheric
origion. Thus the star background is not more than 30 per.cent of
all the intensity. The analysis of the obtained data show that
for the emission in the region of A =5300 R one does not observe
more or less pronounced layers: the glow is connil luou~sly
decreasini from 65 km heiaht up to 130-I80km heights. The low
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layer boundary is not recorded by the apparatus as according
to Plot 3, it was to be located below 65 km.
AA. Comparing the data obtained for the spectrum region of
~,fL,= 9100-10700 R and JL= 8650 , one can see that below
65 km the glow is likely to exist in the both regions. This
may be explained by the presence at low altitudes of the'glow
responsible for the continuous spectrum in the flight sky, This
assumption is eosistent with the absence of the low glow
boundary in thb region of A = 5300
4, Atomic 0xx gen Radiation 0('S) = 5577 ~'.
Analysing the Table one can see that the energy value for
the atomic oxigen green line, obtained from the altitude of
65 km (}), when the apparatus is directed to the zenith, is
equal to the energy value, recorded by the apparatus when its
axis was directed vRrtically down at H = 130 km (~ ). This
testifies to the fact that the glowing layer is situated kaitw
between the altitudes of 65 and 130 km.. The absence of the glow
at altitudes exceeding I80nkm is also proved by the summary aaax
energy measurements recorded in the given filter at the
altitude of 180 km, where the value equal to the Might sky
continuous radiation energy is recorded (see the last Table
line). Analysing the data, obtained when the apparatus was oomi6a
ing through the,layer , we can precise the energy distribution
at the altitudes of 70-100 km: so, from Plot No.4 it is seen
that the J-= 5577 1 glow is originated in the layer, which
has a pronounced lower boundary.
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at 82+2 km and the upper one at H=IIO+IO km, and the layer
gravitation center is situated at H=90?2 km.
5. Sodium Emission ( =5893
Using the same method of treating, as for the line of
=5577Ri we shall obtain the same result; at the altitude of
65 km the energy of E.&tOH equal to 310 R was recorded
by the apparatus directed to the zenith. At the altitude of 130
km this value was only 200 R. This means that the main part of
the glow remained above 130. This conclusion is backed by the
measurements, obtained at 180 km altitude, where the apparatus
directed to the zenith recorded the energy equal to 90 H* This
value is by 20 R less than the difference
characterizing the energy, which the apparatus directed to the
io 6. e
zenit 130 km.
AYYa. s.t is seen from Fig.4 , at altitudes leas than 130 km,
the apparatus recorded a layer, located at the altitudes 70-100
km. According to the sharp glow intensity decrease caused by the
apparatus penetration into the layer, as it was similarly
observed for h =5577 A=8656 R and OH glow, fhe layer gxs~'t
gravitation center is situated at the altitude of 80-85 km. The
lower layer boundary is at 70 km and the upper one is un-
certain.
The analysis of all the obtained data shows that Na glow
is not concentrated in one narrow layer, but it has a peculiar g
glow distribution with altitude: besides the giax layer
located'in the 70-80 km region there is glow at the altitudes
exieding 186 km. Am for the nature of the glow
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distribution in the range of I30-I8u km, it is difficult to
come to any conclusion as the energy radiation value, which
can be concentrated in the air f'egion of 130-180 km is very
small(20-30 R).
6. Atomic Oxigen Radiation 0('D) J,-6300 R
?ig.6 gives radiation distribution with height in the
region of A =6300 R, curve 3 - for the energy value without
background of /hfOH ?
As it is seen from the Figure and the slot, the apparatus,
directed timt to the zenith at 65 km altitude (f) recorded the
value of Ik_tOR =300 R. The apparatus directed vertically
down measured the value 'A+pN =I30 R. at the altitude 130
km (1). Thesivalues are not equal-as it was /observed fQr the am;
emission of =5893 A. The difference Hebb X66 - f/ . /JO
giving the radiation energy value coming from the altitudes axx
exeeding 130 km, is 170 R.
Energy measurements by the apparatus directed to the
zenith at the altitude of 180 km showed that there exists
glow at altitudes exceeding 180 Ian, however the energy. value
fixed in this case is much less than the abovementioned
difference, and it is of 80-100 R. Hence, in the atmosphere
depth in the range of 130-I80 km there is glow in the
investigated spectrum region. As at these altitudes according
to point 10 there is no hydroxile glow, one may conclude,
that the agent, causing glow in the region A p6300 A at the
altitudes of 130-180 km is atomic oxigen 0 ('D).
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Thus 50 per cent of the radiation in the line jk-=6300
induced by the atmosphere glow above 130 km is concentrated at
the altitudes axceeding 180 km,=and 50 bier cent of it -
altitudes in the range of 130-I8o.
Whether there is any glow of A =6300 R below 130 km
it is difficult to decide for certain because of the fact that
the main part of the radiation in this region belongs to
hydroxile radiation the distribution with height of which is
not known. If we assume that in the region of A -6300 R
it is approxematelly the same as that of 9100-10700 R, then
it follows from the data analysis, that below 130 km there is
glow in the line JL =6300 R. This conclusion needs to be
tested experimentally.
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I
Agent Hydroxile
Molecular
Oxigen 02(0-1)1
Continuous
glow-spectrum
Atomic
oxigen 0( S)
Sodium
I Atomic
oxigen 0('D)
ll
9100-I0700 A
8650 A
5300 A
5577 A
5 8 9 3A
6 3 0 0
a(/
:
56
49
38.5
52
79
Y
0.920
0926
0917
0, 26- 0933
71 X30 (4) I8
Y~II I80 (!) t I
Y1D
Absolute glow intencity in Rayleigh
Relative
Intencity
full
by I
5577
EA
CH
I E .,UH
IY
14
21
20 1
I.2 R /A
240
270
250
0
Y
65
(!)
16
2295
185
I R /A
200
300
300
25
72
0
0.4R /A
21095
200
130
2
75
0.4 R /A
0
90
80-I uO
;
U.6h
10
IU
( 170
Energy
difference
Layer location altitudes
layer gravitatio 78 ? 2
center 73 - 2
lower boundary
upper boundary i00 t 2
- 180 - 2 - - ~ ,c tqo
6 b4 e? Q $0-85
-20U-
'
Ib0
> 200
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Fig.I - OH ;low intensity distribution with height
l.- relative intensity, reduced to the zenith;
2- emission in volume units;
3 - photometer indications $rdrtr?Rd which are not reduced to
the zenith.
Fig.2 - glow intensity distribution with height in the region of
8650
I.- relative intensity reduced to the zenith;
2- emission in volume units;
3 - photometer indications, which are not reduced to the
zenith;
Fig.3 - glow intensity distribution with height in the region df
5300 R
1.- glow intensity reduced to the zenith (along the upper
scale - relative, along the l.owrbne - absolute)
2 - photometer indications,reduced'.to the zenith ( here we
have the same scale notation as that for curve I)
Fig.4 - radiation intensity stribution of 5 7 U with height.
1 - absolute glow intensity in the zenith, vpithout background
2 - emission in volume units
Fig.5 - glow intensity distribution with height in the region of
5893 R
3 and 3' - absolute glow intensity, which is not reduced to
the zenith: 3' - summary energy; 3 - energy, without
bhckgi,ound.
Fig.6 - glow intensity distribution with height in the region of
6300 R. j
absolute glow intensity, Without_backgroun4(vhich is not
reduced to the zenith)
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I . L, i~o Bch !~I i o: pliiti;ictric obscrvatio?o of the airL,;low
during the mnter:u tioual Geophysical Year. ^lationc,
bureau of atandarts 5006, 1-33, 1956.
2.1d.I.Cllefov Spektr lnme elektrofotometritcheakie i rndio-
lokatsionnye issledovanija poljarnykh 3ijanii i
avetchenija notchno6o neba. N 2-3 Moskva I960,p.57
3.N.I.Chefcv Spectralnye electrofotometrichesk#e i ra1 o-
lokatsionnye issledovanija poljurnukh aijanii i
svetcheiiija notchnogo neba. N 6 Moskva 1961 p.21
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a
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14M
A9 ~
RJR/
Ow
= 5300 a
O
as so n aA?gM175
V
P"c330PAI K, UAraAOI-&*a%#MA&M uW cdca d"A q
0(S)
1-3377,4
3S
AV
.J
a-C Rant
X-M
+nIl
/r
M ~
7N
Al? -
A5 -
Jww
v is M a t2sE'a
l0 20
Ric I RxrWAMAW ~ r i~Pctl/r~p~1 xf77 roA case.
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Hkm
=5893A
3
110 ~
/40 H
90
80
70
ej
O f Rance
x-'
Xe%. 0
%OO
`o
0
0 L--,- r 1 A l 13) f a.
60 t20 /80 240 3x 360
0 I r 1 1 1~ (J ,
O 60 120 /80 240 JX 360 420 480 540
,04,c.5 ,Dacnpeaene4ue cde4e,4u0 6 cacmu
f =5893 n0 &acome.
T.
A
.AD I
0 (a )
60 1
0 0 120 /W 240'~.A00 00 o/
6000n,0eden6H4e 38
34
0,512
1.1,6
6
0, 56'1
13,1
6r
0,493
r
8,
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IMF,' LC a, 13
1. L.11.Vestine, W.L. Planet Space Sal 1235 /1959/.
2. Uannetio and Solar Data, J. (geophys Ree.66, 1279, No.4 /1961/.
3. Solar Data No.7 /July/ 1953.
4. 1/I1.Nicolet Planet Space Science 5, No.1, 1961.
2/ F.S.Johnion1Ct3ophys Ros.65, No.2,577 /1960/.
3/ A.I.Deseler, S.H.Parker, J. 6-.ophys Rea.64, No.12, 2239 /1960/.
5. P.I.Kellogg. .Y Greods. gees 6S, T~of (1940)
6. W.R.Webber, Nuovo Cimento, Suppl.II, 5 #11957/-
7. Charahchan A.11., Tulinov Y.F. 0 'Charahchan T. N. Xc3T`P 39, ty 8 (ivcol
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CAPTIONS TO FICUI;LS
Fig.1. Detector readings for a part of the flight trajectory of
the third space vehicle, Dec. 1-2, 1960. The upper curve is
the counting rate of the scintillation counter with a thres-
hold of 25 kev. The middle curve denotes the energy release
rate in the NaT (Tl) crystal. The lower curve denotes the
counting rate of the gas-discharge counter.
Fig.2. Distribution of maxima of radiation intensity in the radi-
ation belts, accordin to data provided by the second and
the third space vehicles. Circles denote data for the
second vehicle, and squares udata for the third vehicle,
Grosses derzote the 8 /`'Oi
Pig.3. Radiation distribution in the zone;rdetermined according to
bremsstrahlunr,, from the ':,:e,.iourements made by the second
epaoe vehicle. The numbers on the line of equal intensity
correspond to the counting rate of the scintillation counter
in pulses/am 2sec.
Pig.4. Distribution of the intensity in the zones determined by
the bremsstrahlung, accordin? to measurements obtained by
the third space vehicle. The numbers on the line of equal
intensity correspond to the counting rate of the scintil-
lation counter in pulses/am2sec.
Fig.5. Increase of ionization in the crystal aecordin-) to measure -
ments taken on July 7-9, 1958. On the Y-axis is put the
logarithm of the difference of the observed and the mean
ionization value; observation time is given on the abscissa-
axis. Shaded sections denote duration of the chromospheric
flare, end arrows tho be-inninp and the end of the magnetic
storm. The empty circle denotes the ionization calculated
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from data recieved by Charakchian and others /7/.
Fig.6. Energy release as dependent on distance for the first and
the second space roc' is and for the flight of February 12,
1961.
Fiir.7. D: pondenoe of I on altitude Nlon,r a line of force 26,000 km
distant from the Barth center in the Equatorial plane. I
is a magnitude proportional to energy losses. b.- distance
from the Barth surface.
Dependence of the mean intensity of the bremsctrahlung of
electrons in the outer radiation belt on a certain averaged
intensity of the mznetic field on the Earth's surface, for
a number of regions, according to data obtained on the
second (empty circles) and the third (shaded circles) space
vehicles. The points corresponding to magnetically conjuga-
ted regions are connected by solid (the second apace vehicle)
and dotted (the third space vehicle) lines. Geographical
location of the regions corresponding to the given points
are presented in Table 1.
Fig.9. The region of enhanced radiation in the South Atlantic,
according to measurements on the third space vehicle. Black
circles indicate those points in which protons were observed
by the second space vehicle. Solid lines are for equal
intensity, accordin? to the data of the scintillation
counter; dotted lines denote the parts of the third sjp,ace
vehicle's trajectory; dot-and-dash lines are for equal
intensity of the magnetic field fl; the values of B are
given in oersteds
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- 3 -
Fig.10. Location of the dqu%tor of cosmic rays accordin;; to measure-
ments on the second and the third space vehicle^. The dot-
ted curve indicates the equator of cosmic rays calculated
by Kellogg in the 26-pole approximation.
Fig.11. Planetary distribution of cosmic ray intensity according
to the data of the Second space vehicle. The numbers in
the right correspond to the counting rate of the gas-
die-char!-;e counter in pulses/cm 2see. Dotted lines denote equal
magnetic rigidity according to Webber. Numbers on these
lines correspond to the cut-off rigidity in Bev.
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A"C 9491
200
175
150
125
too
75
aim OZ00 600 04m o5.00 0000 02oo Aoo 0300 1000 ,ioo eoo iioo 14oo oo
tune, hors
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1600
160? 120? 80? 4 U
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? !60?
80
40
40
?
80
X20? 80? 44? 00 40? 80? 120' 160?
c 41
fS
1-71
00 30 f5
\10~ S
30
i5 S S
S 0 0
1S 1,11-4
UU 3
15 700
30,
40D 1S
160` k D 80? 40 0? 40 ?
80' !20' 0?
80?
40?
0?
40?
Boo
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8
0' 16
0' 140' $20' 100' 80' 60? 40' Zo'
?0* 40" I
V' 8
0' !
0"
o' KIV-
ACT
81
I i
4a c=1
130
~S
I
I
r
o o
15
5
15
too
200
15 400
30,
30
15
,
o
V
040? 2
0
0 ,0, 6
0 6
2' h:2' A2
0 !4
0 16
0 /A
O
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AD
9.0
9.O
,magnetic storm
8 9 l0
July
Fig. 5.
Fi g 5
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9 `8!. !
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4
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
E
4C
F'1g7
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
~rl
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
oa
60
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s
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Fig 9
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1
I . . . . i - - I - - 1 - .- I . . . . - !
180 150 120 90 60 50 0 30 60 90 120
West Geogtap/ cae eongaude ?as i
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12-
by V.I.Afanasyeva, J.D.Kalinin
// Solar 6orpuscular Streams by the IGY Ilatall
Undoubtedly, direct measurements with the help of cosmic
rockets are most valuable for investigation of phenomena in
interplanetary space. However, the analysis of ground geomagnetic
data together with geliophysical ones may give some information
about the same phenomena. In particular, it is possible to
determine more or less difinitely the location of solar corpuscu-
lar, streams in space at any moment of time. This is possible
when streams are as far from the Earth as 0.5 astronomic unit.
As long as 1960 one of the authors worked out a conception on
geomagnetic storm families. A storm family was called a pWoup
of geomagnetic disturbances causally connected with one and the
same corpuscular stream. Generally, a family consists of one
geomagnetic storm, in a general sense of this notion, and a
group of weaker disturbances on the previous and the days
following storm days. Sometimes a storm begins a family or
completes it. A favourable location of one of the Soviet magnetic
observatories in Srednikan (Jakutia) helped to expose families.
The presence of two world geomagnetic anomalies - in Siberia and
in Canada - created in Srednikan the conditions of an extremely
vivid alternation of disturbed and relatively calm periods within
storm families. The families.defined by.'the data of Srednikan
were confirmed by the materials of mutualy for away observatories:
Guama, Mirnii, Big-Delta, Littgl-America. Most often activity
within a certain family gradually increases to the middle of the
family and then decreases to its and. The duration of families
are different from 2-3 days to 5-7 days. and more. By the concep-
tions of the authors a family is created by a corpuscular stream
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that has.a relatively narrow most dense core and a very enormous
diffusive periphery. The core may be identified with the stream
in a general sense of this conception in storm.theories. Diffu-
sive periphery is created by the dispersion of the core material.
Streams or their cores may be considered as the geophisics.
used to think distorted in accordance with their radial speed.
A new moment, introduced by the auters into this consideration,
is the account of the values Q,(Q - the differences of 6eliogra-
phic'latitudes widths of streams and the Earth. In other words,
stream cores are those, having 6li6graphic latitudes equal
to the latitudes of active regions on the Sun, which may be
considered as stream origin. Therefore, in most cases stream
cores appear to be situated outside the ecliptic plane and the
Earth passes through the diffusive periphery of the stream and
does not touch the stream core.
On the basis of these conceptions,(a more detailed descrip-
tion of which is published ) the authors gave the analysis of
the situation in July 1959 at the Assembly of the Geodezy and
Geophysics Union in Helsinky [2] , On the same basis one of the
authors succeeded in explaining variations from day to day S q-
-variations by corpuscular effects [3].
At present there is a catalogue of storm families for the
whole period of the IGY. For this period there found out 162
families covering 468 days from the IGY 549 days. As to storm
intensity that is maximum activity in a family, 162 families are
distinguished as follows: 11 families have very large storms
9- large storms and 23-moderate ones. As to the rest 119 families
41 have small storms, and 78 have simple disturbances.
The objectivity in finding out families and their reference
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-to certain regions on the Sun was checked up by the. analysis of
27-day recurrence in families, which the authors and not use in
defining families. It appeared, that 162 families may be ascribed
.to 119 solar corpuscular streams, as a number of streams created
not one, but several storm families (up to 4-5) with neighbouring
rotations of the Sun. If the reference of the families to active
regions on the Sun were subjective, in a number of family 27
day recurrence it would be found out, that in certain rotations
of-the Sun a family::is ascribed to an active region with only
leliographic coordinates, and in other rotations a family from
the some 27 day recurrence is ascribed to the activity in the
other hemisphere of the Sun. However it did not happen. Such a
succession of families appeared to be ascribed to only one active
region. Even more, each family has its own value of At (time
for corpuscular run from the Sun to the Earth orbit) and it
appeared to be like one and the same family 27 day succession
in all the families.
Therefore the authors suggest their family.catalogue, as
a catalogue of solar corpuscular streams, causing on the Earth
during the IGY geomagnetic activity, and in half cases these
streams did not from storms in a general sense, providing only
disturbances and therefore could not be found out in a general
approach to the question.
The figure showed 27 day diagram of all the families. Each
family is given as a triangle. The triangle base is a family
duration, the height is proportional to the maximum activity. The
upper top of each triangle is placed in a divisiorfor days with
the maximum activity in a given family.
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One can note that all the families with very large storms
appeared to be reffered to active regions, whose geographic lati-
tudes are Aq different from the Earth latitude with the averge
. Families with large storms are Q(Q 11467 families from
dcQ . 0
162 were connected with regions with Qc7 *400. The families
with A(q > 260 appeared to be only 6, and only one of them has
a large storm, and the other has a moderate one. Some additional
information about the way of controling the catalogue can be
found in literature [4] . In a table form the catalogue of
storm families was placed in the supploment.The catalogue gives
the dates of family commencements and ends,the dates of the
maximum activity and the characteristics of this maximum activity,
by the scale-very large, large, moderate, small storms and simp-
ly disturbances as well as the dates of passing the central
meridian of the Sun by that active region, to which a given
family is refered, geliographical latitude of this region and
values act and At .
The authors hope, that some investigators will be able
to use the catalogue for the analysis of the IGY data.
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Literature
1. Afanasieva V.I. Geomagnetic storm families and solar
corpuscular streams. Geomagnetism and aeronomy, I Not 1961, 59
2. V.I.Afanasieva and J.D.Kalinin. Solar corpuscular streams
and geomagnetic field in July 1959 Symposium on the July 1959
Events, Helsinki, July 1960
3. V.I.Afanasieva. Corpuscular nature of a day-to day
alteration of calm solar-daily geomagnetic variations.
Geomagnetism and Aeronomy No4,1961, 561
4. V.I.Afanasieva. Geomagnetic storm families during the
International geophysical year. Geomagnetism and Aeronomy, 2 N03,
1962. ( being bonder publication).
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N ' Dates
Commencements
and ends of
family
Maxim. Characters-
activity tics C.M. t~ J At
I 1957 VI-29 3VII 30-VI
2 VIII :5-9 3-VII
3 11-15 12-VII
4 16-18 16-VII
5 18-20 19-VII
6 21-23 22-VII
7 24-26 24-VII
8 27-30 29-VII
9 31-2VIII I-VIII
10 VIII 343 y 3-VIII
11 5-7 6-VIII
12 .'' "' 12-I4 13-VIII
13 17-20 18-VIII
14 20-22 21-VIII
15 25-28 27-VIII
16 29-31 30-VIII
17 IX 2-3 IX- 3-Ix
18 4 4-8 5-IX
19 9-10 9-IX
20 13-14 13-IX
21 15-18 17-IX
22 21-26 23-IX
VG
11
23 IX 29-I-X 29-IX VG
24 X 3-4 3-X d
25 9-12 11-IX L
26 13-15 14-X m
27 x 20-I XI 21-X L
28 XI 1-4 XI 3-XI d
29 5-8 6-XI m
5 6 7 d
29-VI 10?N 70
2-VII 17 S 21
9-VII 10-20N 11
14-Vii 8-10N 4
16-VII 10 S 15
20-VII 8 N 3
21-VII 10 N 5
26-VII 6 N 0
29-VII 6 N 0
I-VIII 8 N 2
4-VIII 10-23 N 10
9-VIII 6 N 0
14-VIII 7 N 0
18-VIII 7 N 0
24-VIII 7 N 0
25-VIII 10 N 3
30-VIII 5-12 N 1
2-IX 7 N 0
6-IX 22 S 29
10-IX 8-18 N 6
13-IX 12-15 N 6
19-IX 10 N 3
21-IX 8 I
26-IX 5-81I 0
I-X 15 N 8
7-x 15 N 9
II-x 15-20 N 11
18-X 25 S 30
I-XI 15-20 S 22
3-XI 15 N 19
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1
2
3
5
6
7
8
30
XI 6-10 XI
9-XI
L
6-XI
150S
I80
3
-I
IO-I6
I2-XI
L
9-XI
7
4
3
.2.
17-19
I8-XI
14-XI
7 N
5
4
j '3
20
20-XI
d
I8-XI
10 N
8
2
34
22
22-XI
d
21-XI
18 N'
16
I
35
23-29
26-XI
G
2 5-XI
I Al
0
I
36
XII 1-4 XII
2-XiI
d
29-XI
15 S
16
3
37
5-7
5-X1I
L
3-X11
15 S
15
2
38
9-13
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L
8-X11
20 n/
20
2
3 9
14-1%
15-X1I
L
II-XII
IO A/
II
4
40
19-20
19-.ELI
L
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22 S
20
2
41
25-27
26-11
d
24-XII
25 S
23
.2
42
30-2 1-1958
3I-XII
G
28-XII
0
0
3
43
1958 5-7
6-I
d
3-I
18 Al
22
3
44
8-10
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d
4-1
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II
5
45
10-14
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7-I
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14
6
LE6
14-16
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I1-I
180 5
15
4
47
1?-I9
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m
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5
7
48
19-20
20-I
L
I6-I
0-IO S
0
4
49
22-24
23-I
L
I7-1
12 N
I?
6
50
25-26
25-I
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I8-I
20 Ill
26
7
51
26-2?
26-I
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25 11
31
5
52
2UO-30
29-I
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9
3
53
30-2-11
1-II
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28-I
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4
4
54
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4
55
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4-11
10 N/
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4
56
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3
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11-13
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8-11
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6
3
58
14-15
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9-II
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13
5
59
16-19
I7-II
L
I3-11
I0 N
17
4
60
19-21
21-II
L
I7-II
5 N
12
4
61
22-24
23-11
L
18-II
84-0
11
5
62
27-28
28-11
d
25-11
10 S
3
3
63
Ill 3-8 111
5-111
L
I-Ill
23 S
16
4
64
9-13
13-LI
m
7-111
15 S
8
6
65
14-16
15-III
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2
66
17-22
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I
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m
22-111
25 A/
32
3
68
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d
24411
25 S
32
4
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
3
y
5
6
7
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30-1 -IY
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20-22
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81
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12
5
83
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3 AJ
7
3
84
12-16
14-Y m 9-Y
8 N
II
5
85
16-20
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20 S
18
4
86
20-23
21-Y d 16-Y
20 S
18
5
87
24-28
26-Y m 22-Y
8 A/
9
4
88
29-30
29-Y m 25-Y
7 N
8
4
89
Y
30-I YI
31-Y v& 25-Y
7 Al
8
6
90
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2-3
2-YI Ly 30-Y
15 S
15
3
91
4-6
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15
4
92
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6-YI m 3-YI
10 N
10
3
93
8-I3
9-YI G 5-YI
10 N
9
4
94
14-16
I5-YI L IO-YI
25 Al
24
5
95
17-19
I8-YI d I3-YI
15 N
14
5
96
19-20
I9-YI d I7-YI
15 Al
13
2
97
20-23
21-IY G I8-IY
15 A/
13
3
98
24-27
24-YI d 22-YI
5 N
3
2
99
28-30
29-YI vd 24-YI
10 A/
7
5
100
YI
30-2 YII
1-YII d 29-YI
0
3
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101
YII
3-6
4-YII L I-YE
9- n/
6
3
102
7-9
8-YII vd 4-Yll
5 A/
I
4
103
9-13
I2-YII d ?-YII
25 N
21
5
104
13-15
14-YII d I0-JII
30 N
26
4
105
16-I9
I8 JII L I5-YII
15 N
IO
3
106
20-21
20-YE
L
18-YII
IO N
5
2
107
2I-23
21-YII
L
19-Y11
4 S
9
2
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
t 2
3
4
5
6
? 8
XO8 VII 24-26
25-:,'II
L
2I-YII
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16
113
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115
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14-15
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d
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16-20
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22
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&
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'1
119
24-25
2 4-Ylil
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8
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26-29
27-Ylil
m
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5 A/
2
121
30-31
3I-YIII
d
28-YllI
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3
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1-2 IX
I-IX
d
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I?
123
3-5
4-IX
VG
3I-Yll
5 S
12
I24
7-10
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L
4-IX
20 N
13
125
I2-I3
I2-IX
d
8-IX
10 S
17
126
14-17
16-IX
L
14-IX
I0 S
I7
127
I8-I9
IS-IX
d
14-IX
I0 S
I7
128
20-22
21-IX
d
I7-IX
10 iJ
3
I29
24-26
25-IX
G
20-IX
20 5
27
130
27-29
27-IX
d
22-IX
IO I
3
131 IX
30-I X
30-IX
L
27-IX
5 S
12
132 X
2-4
3-X
L
30-IX
JO S
I?
133
5-6
S-:L
d
3-X
IO S
I6
134
6-8
I`- X
d
4-A.
15 S
21
135
12-13
13-X
d
`~-X
20 N
14
136
I4--I6
I5-X
d
II-X
20 At
14-
137
16-21
I?-X
d
14-X
IS S
21
138
22'?-''3
-X
m
20-X
4 S
9
139
24-25
24-X
G
22-X
IO 5
15
140
26-27
27-X
m
23-X
IO S
15
141
28-3I X
28-X
L
24-X
7 S
12
~'t xi
I
i-`L1
d
3o-X
15 5
19
143
2-4
XI
2-XI
L
30-X
15 S
19 3
144
6-8
7-XI
d
3-XI
15 S
19 4
145
9-II
I0-XI
d
3-XI
IO AI
7 7
146
11-13
12-XI
d
5-XI
15 n!
12 7
I47
111-17
14-XI
d
I0-XI
15 N
12 4
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1
2
3
4
5
6
7
8
111.8
X!
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I9-XI
16 XI
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3
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2
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2
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15-16
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a
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I
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I57
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7 N
8
2
158
I9-21
19-XII
I7-XII
25 I
27
2
159
22-25
23-XII
20-XII
5 S
3
3
160
25-27
26-XII
23-XII
20 Al
22
3
I6I
28-29
28-XII
26-XII
15 S
12
2
162
30-31
XII
30-XII
27-XII
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I?
3
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 Declassified in Part - Sanitized Copy Approved for Release 2011/12/08: CIA-RDP80T00246AO16600420001-1
1957
duG
SEP
OCT
NOV
DEC
DEC
1958
FEB
MAR
ADD
~ - ' MAY
-~-l-A -JUN
j A UL
~ - a ' a.uc
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DIRECT OBSERVATIONS OF SOLAR PLASMA STREAMS AT
A DISTANCE (1,-1,900,000 KM FROM THE EARTH ON
FEBRUARY 17, 1961, AND SIMULTANEOUS OBSERVATIONS
OF THE GEOMAGNETIC FIELD. t(
61/ K.I.Gringauz, V.V.Bezrukikh, S.M.Balandina, V.D.Ozerov,
R.E.Rybchinsky.
Abstract
Final results are presented of the processing of the
data of the experiment aimed at investigating solar plasma
streams from the Venus probe launched on. February 12, 1961.
Preliminary results were 'reported by K.I.Gringauz at
the Second International Space Science Symposium in Florence
in 1961.
The results are compared with the geomagnetic field
simultaneous observations.
In K.I.Gringauz' report at the Space Science Symposium
in April 1961 in Florence (1) the preliminary information-
was given on the results of the experiment carried out by
means of charged particle traps on the Soviet Venus probe
launched on February 12, 1961. In the present report final,
somewhat corrected results of measurements are presented.
They are compared with the results of the simultaneous regis-
tration of the geomagnetic field variations on the tarth.
Let as remind that at the said probe two three-elec-
trode traps were installed among the scientific instruments.
They differed only by some design changes from the traps
mounted on Lunik II by means of which in 1959 solar plasma
strearJs were recorded for the first time outside the geo-
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magnetic field (2). The changes introduced into the design
were directed to the reduction of its weight and further
decrease of the collector current component produced by
the photoelectron and secondary emission from the inner
grid of the trap.
The potentials of the outer grids of the traps on the
Venus probe were 0 and q _ +50 volts . During the
measurements the traps retained definite orientation with
respect to the direction to the Sun and to the velocity
vector due to which collector current variations caused by
the body rotation described in (2) and (1) could not take
place,
Fig.l gives the results of the measurements of the
trap collector currents during three radiotelemetry trans-
missions from the Venus probe. Table 1 gives the time t
of the beginning of each of these transmissions and the
distance R of the probe from the Earth's centre which cor-
responds to the beginning of the radio contact.
No.of Transmis- 't (Moscow Time) R (Km)
sion Received
1
12.11.1961 6h 45m
30,000
2
12.11.1961 14h 25m
170,000
3
17.11.1961 14h 35m
1,900,000
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While considering Fig.l one should bear in mind that
the collector current amplifier with the outer grid poten-
tial equal to 0 had a characteristic which consisted of two
linear portions. The slope of the upper portion was com-
paratively low. The maximum measured current was close to
8~..Q10-8 amperes. The trap collector current ampl if ier with
I , L -t50 volts had a characteristic close to linear one.
The maximum measured current was equal to 2.10-9emperes.
As it should be expected the collector current modu-
lation, which took place in previous similar experiments,
was absent in this case, as is evident from the graphs of
Fig.1.
Let us note that the recorded currents are somewhat
lower than those determined by the positive ion fluxes get
into the trap at the expense of the currents produced by
the emission of photoelectrons from the inner grid. How-
ever, from the materials given in (1) and (2) it can be
seen that the photocurrent from the inner grid in the traps
on the first space probes did not exceed 5.10-10 amperes,
while in the traps on the Venus probe it was considerably
lower, since the inner grid transparency was increased.
During the first reception of signals the -currents of
both traps oscillated near zero values. The Venus racket was
at distances of 30,000 = 45,000 km from the Earth's centre,
i.e. in the outer part of the second radiation belt. The
absence of considerable negative collector currents in the
traps during the first radio contact,testifies once more to
the absence in the second radiation belt of soft electron
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fluxes on the order of 1010 cm-2 sec-1 postulated by the
majority of the investigators of this belt in 1959-1961.
A more detailed consideration of this problem is given in
the report by Gringauz,' Bal a.nd ina, Bordovsky and Shutte at
the present symposium (3).
During the second radio-contact low positive currents
were registered in both traps. Considerably larger currents
were recorded in the traps during the third radio contact.
The current of the trap with the outer grid potentiaa_
+ 50 volts is equal to 2.10-9 amperes, i.e. corresponds
to the maximum value of the current which could be recorded
by the collector current amplifier of this trap. The simul-
taneous current in the trap with the zero potential on the
outer grid is equal to 3.3.10-9 amperes. This value ap-
parently determines the N+ value of the positive corpuscular
stream which ID ok place during the third radio contact,
namely .-109 sec-2 sec-1. With the accuracy up to the measure
ments errors the stream value was constant during the third
radio contact.
During the third reception of signals a magnetic storm
with a gradual commencement took place on the Earth, which
started on February 17 about 12 hours Moscow time and lasted
for several days,
Fig.2 presents collector currents graphs in the traps
for each radio contact on the same time scale and the results
of the simultaneous registration of the magnetic field
parameters according to the data of the Central Magnetic
Observatory (Moscow). The latter represent the records of
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the Lacourt magnetograph recorders which registered the
geomagnetic field intensity horizontal component H and
the angle of the magnetic declination D.
The problem of the correlation between the intensity
variations of solar corpuscular stream affecting the Earth's
magnetosphere and the geomagnetic field variations during
the magnetic storm produced by this stream is not suffi-
ciently clear at present.
Some of the authors believe that fur the first hours
of the magnetic storm the geomagnetic field fluctuations
corresprnd to the fluctuations of the corpuscular stream
and then thee correspondence is violated due to the action
of the electric current systems which appeared in the
ionosphere under the influence of corpuscular streams (4).
Ttis would have been checked up if we had had at our
disposal simultaneous long time observations of the cor-
pupuscular stream variations in interplanetary space out-
side the geomagnetic field and of the magnetic field varia-
tions on the Earth. Due to the shorttime (half an hour)
duration of the third radio contact the experimental re-
sults obtained from the Venus probe have not provided us
with such an opportunity.
Nevertheless it is interesting to.make an attempt at
establishing the correlation between these values assuming
that the geomagnetic disturbance value is determined at
this time by the corpuscular stream getting into the Earth's
magnetic field. It is necessary to take into account that
between the moment of the registration of the density of
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some part of the corpuscular stream on the probe and the
moment of the contact of the same part of the st re an with
the Earth's magnetosphere some time has elapsed determined
by the mutual location and mutual velocities of the motions
of this part of the corpuscular stream, of the Earth and
the rocket.
Fig.3 presents the mutu al location of the Venus probe
and the Earth during the third radio contact. The Venus
rocket was at a distance of 1.89 million kilometres from
the Earth. The distance from the Sun to it was by 1.54
million kilometres less than the distance from the Sun to
the Earth. At the same time it somewhat lagged behind
the Earth in its angular motion about the Sun.
It should be borne in mind that the tangential velo-
city of the corpuscular stream motion at a distance of
1 Astronomical Unit exceeds the Earth's orbital velocity
by a factor of 14.
Trying to estimate the delay of the moment of the
contact of some region of the streanwith the Earth relative
to the moment of its contact with the rocket some supposi-
tions about the stream shape should be made. This stream
region can come into contact with the Venus probe and then
with the Earth by its front ( the time C of the delay of
these phenomena will be determined by the radial velocity of
corpuscles), or by its lateral surface (in this case r
depends also nn the stream tangential velocity equal to
^' 400 km/sec.). Cases are also possble when this
region of the str. eam comes into contact with the Venus
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probe by its front and with the Earth by its lateral sur-
face.
The radial velocity (V rad.) roughly estimated from
the delay of the moment of the beginning of the magnetic
storm relative to the moment of the passage of the active
region on the Sun through its central meridian turned to
be equal to 400 km/sec for the storm on February 17,
1961.
Taking into ecco ant all these suppositions the time
`r turned to be within the limits of 64-110 minutes.
The boundaries of the hatched area in Fig.2 are determined
by the moments of the beginning and the end of the third
reception of the signals with the greatest and lowest delay
time taken into account.
In this region and its closest vicinities the H fluc-
tuation reached about 100 gammas.
It shoull be noted that the value N+ measured by us
is close to the maximum value N+ obtained in the experiment
by Bridge, Dilworth and others (5) on the Exploeer %
satellite, and the velocity of corpuscles determined by
the indicated indirect method is close to the corresponding
meal value directly measured in the experiment (5).
Acknowledgment
The authors are grateful to V.I.Afanasyeva,
Yu.D.Kelinin and E.R.Mustel for fruitful discussibn.
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References
1. K.I.Gringauz, Space hesea.rch II, 1961, North Holland
Publishing Company, Amsterdam, p.539.
2. K.I.Gringauz, V.V.Bezrukikh, V.D.Ozerov and
R.E.Rybchinsky, Dokiady Akad.Nauk SSSR.
Vol.131, 1301,1960; "ISkgsstvennye Sputniki Zemli",
The Publishing House of the USSR Academy of
Sciences, 101, 1961.
3. K.I.Gringauz, S.M.Balandina, G.A.Bordovsky, N.M.Shutte,
The Report at the Present Symposium.
4. V.I.Afanasyeva, Proc.of the Institute for Terrestrial
Magnetism, the Ionosphere and Radio Wave Propa-
gation of the USSR Academy of Sciences, 12 (22),
63-67, 1957.
5r H.S.Bridge, C.Dilworth, A.J.La.zarus, E.F.Lyon, B.Rossi
and F.Scherb, Direct Observations of the Inter-
planetary Plasma., Report at the Kyoto Conference,
September, 1961.
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( { , i T
Mogilevsky E.I.
// Corpuscular solar streams with
forceEi'ree magnetic fields(
1) In the hypothesis given below one has made an attempt to
find out some main properties and the structure of a corpuscular
stream from the observational data and the analysis of plasma
movements in active regions of the Sun with a bipolar magnetic
field. The magnetic field of such a stream, whose energy exceeds
the kinetic energy of the stream, is not a frozen magnetic field
in a stream 3lasma, but a rpdce free field of a closed system
of the stream plasma. The stability of such a stream and main
features of interaction of it with the magnetosphere and ionos-
phere of the Earth are determined not by a stream plasma, but
by the direct influence of a forcilfree magnetic field of the
stream.
2) Recent numerous observations of the Sun prove that all the
combination of complex phenomena in the active regions on the
Sun is determined by the development of local magnetic fields.
The generation and outcome of geoeffective corpuscular strecros
are also determined by varying local magnetic fields. In the
region of the geoeffective stream origin ( upper chromosphere
end the corona) the magnetic field can appear only as a result
of a successive movement of chromospheric plasma clouds, carrying
its own magnetic,field [1 3. The outcome of the magnetic field
into the corona as a result of wave processes and diffusion is
non-effective [1,21 . As a necessary consequence of chromos-
pheric-coronal plasma compressibility, the conditions of Helm-
holtz movement are not valid when the plasma is moving. As a
result the plasma cloud moving into the corona obtains its own
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forcefree magnetic field [1 ].
A forcefree character of the magnetic field of a plasma cloud
is also seen from the analysis of the conditions of the stability
of the current system with the spiral symmetry, arising in a plas-
ma cloud moving in the outer bipolar magnetic field of the active
region. The field of such a cloud reminds us of a magnetic field
of a stellorator. It the characteristic sizes and density of a
plasma cloud with the magnetic field exceed the critical values
L> 10' c~ then such a cloud moving in the
corona does not decay and may go radially outward to the direc-
tion of the Earth. By twisting a toroidal magnetic field of the
plasma cloud, arising in moving in the outer dipole field, the
current field is strengthed up to --50 gausses at the cloud
boundary. A relatively large magnetic field and its fordfree
character guarantee a cloud stability. in the solar corona region
and in its movement in an interplanetary space. Magnetic fields
of active prominences may serve as an analogy of such magnetic
fields in moving plasma clouds. As the observations [ 3,4] show,
the magnetic fields in moving streams of prominences achieve
several hundred gausses. It corresponds to the condition of a
-onsiderable excess of the magnetic field energy over the kinetic
energy of the stream. In generating a plasma stream with a suffici-
ently strong forcefree magnetic field in its environment an
acceleration of a certain part of quick thermal protons, and
electrons of the Maxwell tail becomes possible. Electrons accele-
rated up to energy of several dozen Mev will give synchronous
radiation (radiobursts of type IV ); accelerated protons, trapping
into the magnetic field of the stream, come together with the solar
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stream to the Earth magnetosphere and cause polar blackouts, For
rather weak magnetic fields of the stream (for instance, uncon-
nected with chromospheric flares ) such a process of generation
may appear non-effective.
3) It is necessary to underline that a plasma cloud with the
forceeree field differs principally from the moving plasma with
the frozen magnetic field , connected with the Sun, as it. was
cbnsidered in a number of papera{ 5 ]. The authors of this
works have not determined the energy, necessary for stretching
the magnetic shell with the plasma over the distance of at least
dozens of astronomic units. The exact solution of such a task due
to its non-linearity, is very difficult, and even an approximate
estimation shows that the process of magnetic envelope stretching
into an interplanetary plasma requires the energy of many orders
greater than the energy of the active region on the Sun E11 6 3.
Even these facts are sufficient to refuse the model of a corpus-
cular stream in a form of a expanding shell. Besides the long-
-existing corpuscular stream with a stretched magnetic shell
should turn into a very twisted spiral due to a solar rotation
The Solar corona structure, investigated in detail during solar
eclipses, does not indicate to the presence of any twisting of
the coronal streamers. All these difficulties are naturally
dropped off for the corpuscular stream model, consisting of a
number of plasma clouds unconnected with the Sun. Then current
systems from fordfree magnetic fields, For such a stream it is
possible to calculate a disturibution of a density and a simpli-
fied picture of the magnetic field. Such a calculated scheme is
presented in fig.I.The interaction of the stream magnetic field
with the magnetic field, of the active region on the Sun determines
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4
kinematics and energetics of all plasma cloud succession with the
forcel--ree field, composing a geoeffective corpuscular stream
[ G7 ] . Fig. 1, shows, that in a case of plasma clouds with
forcelfree fields the effect of a reverse correlation between the
strengtk,t of a magnetic field and the value of a concentration
of a stream plasma should be noted. In the region of the plasma.
"core" itself (region A')', where we have a system of weakly
decaying currents, the magnetic field is almost absent and vice
versa in region B, having a ,,;eater volume where we have a magne-
tic field, the plasma density is minimtun. In region B , like in
a magnetic trap, there might be highenergetic protons of solar
tF.:G io
cosmic-rays (particularly soft cosmic rays ). Simultaneous
measurements of plasma concentration (or plasma flux) and the
magnetic field, which have began being made by means of cosmic
rockets at substantial distances from the Earth, can allow to
solve a question whether the stream is a plasma with a frozen
magnetic field (as it is usually approached) or our s-cheme is
true. Such measurements on the Soviet cosmic station., flying to
the Venus 181 and on the American Satellite "Explorer X" indica-
te to the correctness of the model considered. Under the condition
(5 ,.r,alh IK,;? the plasma stream with a forcifree magnetic field of
the structure considered goes through a rarefied interplanetary
plasma almost without essential changes. A certain decre-
ase of the current intensity in a plasma "body"of the stream will
bring to a decrease of the magnetic field strength, but the
character of the field remains forceJree.
41. As it is known 19 ,, the plasma stream moving at an
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ul.tra:,oriic ;p, od1 ii:, one interaction with the Earth magnetosphere
flows round it, causing the effect of the field "compression".
An explanation of penetration of the stream plasma even into
outer parts of the magnetosphere comes across a number of prin-
cipal difficulties, In the considered scheme a forceeree magnetic
field of an impinging stream causes essential effects in the
magnetosphere long before a possible penetration of the stream
plasma into the magnetosphere. In the first approximation this
influence may be described by the consideration of the impignent
at an ultrasonic speed of the side and fore front of the stream
magnetic field. The latter may be considered as a movement of
a quaziplane magnetic piston in the outer plasma of the Earth
exosphere. In this case the interaction of the stream field
with the magnetosphere causes longitudinal and transverse waves,
travelling to the Earth surface. The scheme of the geomagnetic
field disturbances, is like the one considered by Piddingtonli0]
The calculations show that longitudinal weak shock waves carry
the greatest flux of magnetic energy. A somewhat less flux of
energy will be connected with transverse waves. As in the consi-
dered scheme the energy of a f'orce'ree magnetic field of the
stream 2=3 orders exceeds its kinetic energy and a very effective
transfer of energy from the stream takes place,so only in this
case an energy of ~-l0Z6: to eZ~s ( that is sufficient to
cause a geomagnetic disturbance) can be transferred to the Earth
magnetosphere. A number of peculiarities during geomagnetic dis-
turbances and disturbances in ionosphere connected with them
can be analysed in the light of the scheme considered.
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Ttl a cpaTypa
I...~ortute3C1 D 3.YI., I'eor.1~I'IIUTIt3,1 1 aopoiiOrmSI, I9 1 ,
I, 1:, 2, 153
Ootorbock D.N., Astrophya.J.,196I, ,347?
3. iiUiiii'i l x.A., I'e0f.IarIIeTIImrs ii aDp)OI.Or:iIIfI, 1962 , 2 ( }3 II011).`1rLi) ?
4, Zirin H.,a.A;B.Severn`y, The obaervator7,I96I,?I,
N 923, 155.
5, Piddin ton J.II., I'hw.Rov.I 53,iL?_, 5:%9.
T.Go1d, rIuovo cimento,1959 ?i, Si1PPl .tlo .1, 318.
Aj3trophya.J.,Suppl.Ser.,1960,4, 406.
re(x::u.10T:7:jh Ii 3OpOI10r.1iI, 1962, 2
( B nOLlaTHH ).
'7. r OrIL7ICI3CI{IIiI 3.11. 11). IuI-Ta 3CC:.;H OAX) :daminu3t:k3 (IlL a1),
IWI, Bit. 6 (IG.), 3.
Co AO,nrltxOB C.111., ~y3ros JI.H., Ylpouteimo E.I'.. reor.larlicm I
Ii aopo1Ior ul, 1962, & ( B netk3TI4)
913.11. LJJI COOP, E5'9, 124, 5, 1001; 1269 1' 3, 52I.
10. Piddington J.H., M2on.Not.R.A.5.,1955,II ,671;
J .Geoph .Rocs . , I960,?j, N'I, 93.
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by .1:. Polo:~kov, A. E;.Mikirov
,29,
41 ELIEC1'1W0!'H0910METTRRY 01' 1'kU CHOS I. iic;GIO['T OF OU''EII SOLAR
COiZCi1A IN 211E VISUAL SPECTI:UIs aEGION DUdNG '1'IIE FULL
SOIAI: 1J-JLItSI: 01? PEB1LA1 Y 15, I96I.`'
The aim of the experiment was an investigation of brihtness
distribution in the visual spectrum region close to the Sun
space, including the outer corona, than investigation of brightm,
ness distribution in the visual spectrum part of the outer
corona and the sky region enveloped with measuring.
According to4 the spectrum, measurements cover the range
from 3200 to 6200 R. Further it was supposed to measure the sky
region begining with the Solar edge up to the distance equal
to 28Re
As the container orientation turned out to be different
from that of the calculated one another Solar corona part had
been measured.
Supposed and really measured Solar corona regions are
presented in Fig.I.
Measurement Methods
Measurements were carried out by means of electrophotomete3
" Z OnC-2", given in Fig. 2.
Electrophotometer "X,/C-2" is a camera -obscura with
f=44 mm in which a picture of the investigated sky region is
projected on a photocathode.
The 0,19 x 4.2 mm slit, that corresponds to angle
dimensions of 0.15 x 5.50. gradually moves before the photo-
cathode.
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The scanning slit makes a reverse - progressive movement.
A slit movement direction is shown by an arrow in Fig
..2. During
variations cycle which goes on for 2 sec., the slit manages to
scan 140 in progressive and reverse direction. A disc with holes
is placed before the alit what permits to modulate the coming
radiation with the frequency of 247 c.p.s.. A photomultiplier of
" 9Y-25" type with qn antimony-zesium cathode sensitive to the
0
region of 3000-6200 A ,e.g. sensitiv to that region, inside of x~d
which the maximum intensity of the scattered radiation is
locatited, is used as a receiver of the radiation.
A signal taken from the cathode follower comes in to the in-
let of the telemetering system.
The instrument calibration was produced on bench photometers
A standart lamp was used as a light source with( a known light
intensity and colour temperature Q2800?K). A light filter of "C"
type, turning the source temperature into a colour temperature
6500?K was put before the light source.
The instrument was placed at a definite distance from the
light source. A frosted glass with a known trasmission coeffici-
ent was placed before the instrument. The frosted glass
brightness, measured by the instrument while calibrating,
varied within necessary limits with the help of light filters
of "HC" type.
The instrument can measure brightnesses from 4.I0-7 to
1.6 ?I04 stibls, i.e. in the range of throe orders of
brightness variations.
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It is known that the total brightness of the solar corona is
of the order of 1.5 .10-I stilb, consequently the instrument
at the suggested orientation has to be.scaled out up to the
distance of the order of several solar radii and to measure
brightnesses'at the distance from 10 and more solar radii..
Actually the orientation turned out to be different but as
useful as it could be at the actual picture of measuring, and
a very interestincorona region from II to 33 Re. was
measured (see Fig.
Measurements Results
Measurements results are given in Fig.3. What conclusions
one could colpe to considering the obtained results? At first
let us igssume:, that the results given in Pig.3, Illustrate the
brightness distribution in the region from II to -33 Re, which
are burdened neither by instrumental errors nor by other
disturbing effects.
This problem concerning instrumental errors on other
considered
possible disturbing effects will be partially later. So, let
the observed picture of the brightnesses be corresponding to
outer
the ,brightnesses of the observed? corona; region when the
photometer slit is moving over it . If it is so, the only assn
possible conclusion from these results may be the one, that the
outer corona is presented as an extremely inhomogeneous
formation with the size of inhomogeneities of the order of 61
of are (in grade dimension) that corresponds to 280 thousand lit
in the unbar dimension.
What bases is this conclusion put on? Really, let us assume,
that the scattering substance is distributed in such a way, that
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scattering radiation intensity (the corona brightness) falls x4xx
equally (isotropiccally) according to a certain power low,
let it be according to the law of /' S (where JQ - is the
distance from 0 to the scattering light element of the
volume). or according to some other one (power law). It is clear,
that even at the uniform distribution in light scattering
substance space this brigthness decrease will occur according
to the law J 1, and for gradually decreasing density -
according to another low apporximated by higher powers at )
If we assume it then at the described scanning by the
slit, of the corona region , it is easy to show that we are
to obtain the following picture (theoretical one) of $
brightnesses variations; a measured brightness should vary accor
ding to the bosine law (in the corresponding power), i.e.
inside of the measured region, if ? is varying according to a
power law. i.e. if oC angle is read as it is .shown in Fig.I.
However from Fi;.3, we see, that theoactualndicture of
e
brightnesses variation does not completely to the theoretical
one . Only at some moments we hate measurements rugione, where
brightnesses variation is like the cosine curie variation.
Further more, from Fig.3 we see, that in some cases
instead of expected intensity increase a considerable decrease
is recorded in general it has no strictly regular c aracter.
However, the maximum kind minimum values correspond to' these ones
which were expected according to Van de Hulst:
The maximum for values of Ro = II
and the maximum value for values of Ro = 30
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For a coin prison we give brightness data from Vu.i ue
mast and Bluckwell t s work /1/, /2/ (see Fib;-4).
What does it testify to?
We believe, that considering all the obtained results,
evidently one could come to the only conclusion, that
substance scattering the light in the outer corona is'distribut-
ed extremely inhomogeneously, i.e. it has inhomogen:e'ous
structure with inhomogeneiti49 sizes less than 6' of are.
Angular sizes of the inhomogeneities (6' of arc) are
obtained from the used brightness measurements method:,
i.e. a sycle of measurement is, equal to I seg. For this time
at the used telemetric methods (125 information at I see) a
record of 125 brightness estimations is obtained 4.e. 125
points in Fig.5). It is clear that from point to point the
slit manages to cover the distance equal to 6'.
The conclusion, that the outer corona has a inhomogeneous
structure, generally speaking, corresponds to that one, which hai
been made in Vitkevitch's work /3/, concerning the so called
suppercorona of the Sun, observed by radiotechnical methods,
during a solar eclipse of Crabe nebula.
Those measurements concern the same distances from the
Sun, as in our case. The inhomogeneities in the suppercorona
ob4usly,describe jet character of the solar corpuscular
fluxes, forming electron-isotopic suppercorona.
Thus, according to V.V.Vitkeviteh's data, though they were
made with hiegh decree of reliability, one can judge only of
electron inhomogeneities sizes. While our data, ceneri~.Ily
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speaking, concern both scattering on the dust, and scattering
by free electrons. At first it seemed, that only dust substance
of interplanetary component is responsible for the light
scattering at this region, if we are of the same opinion as
that of Van de Flulst /1/, /5/.
Howadays, these ideas are additionally considered in
Blackwell's works. However, dust component contribution into
the outer corona brightness in the main one and it comprises
90 per.cent. of the total brightness. So, scattering on the
free electrons comprises less than 10 percent of the total
brightness.
Consequently V.V.Vitkevitch's results may be compared
with ours, but it hardly should be said that these tli.eae works c
confirm each other. It would be seccurer to say that obtained by
us results about the outer corona structure and inhomogeneities
sizes in it do not controdict to V.V.Vitkevitch and Havish's
ones /4/.
W1&Lile considering the reliability of the obtained results
we looked through possible effects, which could influence on the
results. It may be light from other possible light sources (not
of the corona) and instrumental errors.
Only of the own lumenocity and the aerth atmosphere
brightness in the region of a complete shadow and possible
black out eaused by ring of dawn were considered from possible
strange light sources. There is no other hinderances.
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It appeared, that possible hinderances and instrumental
effects do not exceed by its value 10 per.cent. of the
measured brightness value, e.i. I0-7 stilb.
Thus, the conclusion concerning the inhomogeneous
structure of the outer corona, apparently, is true,
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REIN ERENCES
I.H.C. van de Hulst Ap.J. 105, 471, 1947
2.D.E. Blackwell, M.N. 115, 629, 1955
3.M.F. Jaghom, M.N. 122, 162, 1961
4.V.V. Vitkevitch
5. "Solntse", IL, 1957, p,225-24I
6.A.E.Mikirov, DAN, 142, N3, 1962
7.V.IpMjukhjurja Trudy GGO,,byp. 93, 1959
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2.z
z( .
l y G.S. IVArTOV-KHOLODNY, G.M. NIKOLSKY.
(l PREDICTION'AND IDENTIFICATION OF EMISSION LINES IN THE
SOLAR EXTREME ULTRAVIOLET 1100 ~.~
The solar extreme ultraviolet radiation intensity definite
ion is of paramount importance to understand. ionization,
excitation, heating and other physical processes in the Earth
ionospere, in interplanetary media, and In the Sun atmosphere.
Recently direct rocket measurements of the solar extreme ultra-
violet and X-ray radiation power have been a great success and
gave some results, however they are faced with certain
experimental difficulties when carrying -oust absolute energy
measurements in rather various spectral regions. It is a th-:ory
that should contribute in overcoming these difficulties.
j$eL.tral investigations gave especially important information.
Beginning with 1958 a number of spectral rocket meuaure-
ments of solar radiation in \- 1100 R region were carried out
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and about 200 emission lines were recorded. Solution of the
solar extreme ultraviolet spectrum is one of the most interesting
problem resulting from modertirocket investigations and raised
before astrophysics and spectroscopy. Though many attempts
were undertaken but up till now one had succeeded in identifying
less than a half of all the observed lines and more than a
half of identifications undertaken by various authors were not
consistent. Evidently one could come to final conclusions
concerning the correctness of identification only after the
analysis of the line intensities and to do this we should have
a certain comprehension of physical conditions in the transition
layer and in the solar corona.
I. PREDICTION
The authors in paper /1/ established line theoretical
intensities of the solar extreme ultraviolet. Radiation intensity
of a certain ion in the corona and in the transition region
between the corona and the chromosphere can be defined by
generalized measure, pf emission
U*Itl _%t
AT= h c,, rr ,L
k(r)
where neT - electron concentration and temperature; h(TT) and
h(T2) - layer bounderies, where this ion emits. To plot A (Ti)
1.
'
as a function of the ionization temperatureYiii the whole
interval between 104 and 106 bK experimental intensity estimation
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of 27 sufficiently bright reliably identified lines were used
as the initial d ;te. These lines were arranged in spectral
regions around 1J.,4 line. Ti, Tl and T2 temperature values
for each ion were estimated on the bases of the developed
ionization theory. It was adopted that excitation is resulted
from an electron collision and it is balanced by spontaneous
transitions. In most cases information about oscillator
strength is not available, therefore approximate values were
taken for them. The use of f'tT) function gives an
apportunity of calculating spectral line intensities without
any knowledge of a transition region model. It was considered
thet all the suitable ionization stages of each element
and all the atomic transitions for which Laport's rules and
selection rules are true. In work /l/ there was presented'
the total list consisting of 480 most bright emission lines
which are to be observed in the solar extreme ultraviolet
spectrum 20 - 2000 R and about 400 lines of them are in the
spectral region =1100 A.
II. IDENTIFICATION
Theoretically predicted lines and their intensities were
compared with experimental spectral data concerning the solar
extreme ultraviolet radiation obtained by rockets. Work /2/
by Violett and Rense gives wave lenghts and visual intensities
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"i" of 130 lines in the spectral region 84-1160R. Works /3,4/
by Hinteregger present photoelectrical spectrum records in
absolute units of energy, where one can find 180 lines in the
spectral. region 60-11.00 R. Wave lengths for those lines were
estimated by us only approximately. Though the most bright lines
were observed by all the authors mentioned before together, there
exist however non-consistences even among bright lines, and the
matter might be cleared out only with the help of a proposed
line prediction. It appeared that there are several false lines
both in Violett and Rense's /2/ spectra ( evidently because of
a low quality of spectrograms ) and in Hinteregger's /3,4/ the
latter is probably connected with.fluctuatikons of the background
and the influence of the absorption bands of atmosphere molecu-
lar nitrogen and water vapour released by a rocket and apparatus.
From the total number of 225 lines, observed in /2/ and
/394/ we managed to identify 180 lines with the help of the
predicted list of lines /1/. Thus almost all really observed
lines were identified while more than a half of unidentified
lines were simply false. It should be emphasized that all the
most bright lines predicted theoretically were recorded in Violet
and Rense's spectra and in Hinteregger's record. However several
extreme ultraviolet lines belonging to Ca XII - XV, A XI etc.
which have too high ionization potential - 669-800 ev were
not recorded. The results of the identification of the?obuerved
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lines are presented in following Table 1.
In Table I "?" - marks the lines, which are likely to be
false; "+?" - marks the questionable identifications for which
the wave lengths are available but theoretical intensity estima
tions are more that an order of magnitude less. As far as the
data of Table I are concerned the following should be pointed
out. In the solar extreme ultraviolet spectra the most abudant
elements H, He, C, Ne, Mg, Si, and Fe were observed at all the
ionization stages up to the coronal stage, and lines of more
r4re elements N, Al, S, A, Ca, Ni were observed as well.
Probably further experiments will give an opportunity of
observing weaker lines the list of wave lengths and expected
intensities of which are given by the authors in paper /I/.
Among the experimental data of works /2/ and /3,4/ we can
find many / . 15/ lines observed in the second and third
orders as grazing incident spectrograph was used. Examination
of Table I data shows that the discrepancy between Violett and
Renee's /2/ and hintere ;er's /3,4/ experiment--l data is more
distinguished in the region 500-1000 H than in the region
500 ~. Line identifications are also poorer in the range
500-1000 q and this we can probably connect with the fact that
these experimental data are lest reliable (compare the regiofl
850-958 A where N2 bands fall). From all 180 identifications 40
ones, which belong to weak lines, are considered to be q,_tcstion
able though they may turn out to be true. Almost half
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-6.
of the latte*lines ( 20-30) which have-net-befuttident.ified,
by--us'-an~ cannot be considered false are probably not identified
line estimations
because of incorrectness of their theoretical intensif V(aabsence
of data about terms and oscillator strenth of some ion, and
imperfection of ionization and excitation theories) or the
matter can be connected with intercombination transitions which
were but little considered in /1/. Chus from 4 intercombination
transitions for coronal ions indicated by Pecker and Rohrlich /5/
as it is shown in Table 1 three of them correspond to the observ-
III. RADIATION INTENSITY
On the bases of the proposed prediction and, line identificat-
ion one can estimate the flux of the extreme: ultraviolet
radiation of the Sun and that is of great importance for
understanding ionizations processes both in the Sun (chromosphere
.:and solar prominences) and in the ionosphere and also in inter-
planetary space. A comparison of theoretical /1/ and experimental
/3-4/ data concerning the reliably identified line intensities
seen in Fig. 1, shows that these data in the spectral regions
60-200 R and 900-1100 R mainly did not differ more than a factor
of 2-3. This testifies particularly to a high accuracy of a
prodiction of line intensities in /1/. In the X-ray range 60-200
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intensity estimations agree at average with results of rocket
measurements carried out by means of photon counter;/6/ and
in the spectral range around they agree with available
rocket measurements of line intensities., which were used in
there is
computation of theoretical intensities. Thus a-possibility of
correct conftrontation of solar radiation intensities in rather
various spectral regions theoretically. However, in the spectral
region 200-900 R in Fig, 1 one can see d systematic variation
of the ratio of the observed intensties to theoretical ones.
As far as it is difficult to expect a systematic variation of
theoretical value ray with a wave length, it``id~s probably connect
ed with the fact that spectral apparatus sensi~Gity variations
were not carefully taken into account. According to Fig. 1 the
1-t.3-
apparatus sensivity in 250400 2 is. - 1 - 1.5 orders less than
that accepted in /4/. It might be induced by absorption in the
atmosphere layer overhead the rocket during spectrum record
or by water vapour released by design details situated near
the light beam. The letter is more possible as the maximum in
the water vapour absorption spectrum is also situated in 250-400
R /7/. The conclusion concerning the influence of effects of
absorption of radiation upon experimental data is also justified
in Violett and Renee's data , as it is seen in Fig. 2. It i.,
clear from Fig. 2 that visual intensities g&e also under -
estimated in the region 250-490 R if compared with theoretical
intensities.
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Corrected for an a:,bsorbtioa effect the curve o. L,veru cd
sac tral erisrg;y distribution in the solar eytrei;,e ultraviolet
w,is plotted in Fi,g, 3. Points of the stepped curves in Fig. 3
are obtained by averaging theoretic~wl intensities of all the
lines /I~ according to wave length intern als of n,\ = 50
and circles. are obtained by averaging the identified lines
presented in Table I. I,s the both data for 460 ? coinside
mainly all the strong lines are identified in this spectral
region.
Spectral energy distribution in extreme ultraviolet of
the Jun reveals the maximum in the region 200-400 P with power
density 0.05 erg/sm2sec 1., This radiation originates from
the upper layer of the transition region. The main part of the
solar extreme ultraviolet radiation energy is concentrated in
200-400 L', near the Earth this energy is approximately
equal to 7.5 erg/sm2sec. Besides the gross maximum in the
region 200-400 one can notice several maxima more in Fig.3
in the wave length region, 60-100, 550-650,750-850, and 960-
-1050 R. To precise the spectrum structure in the region _400
averaging line intensities according to the spectrum inter -
vals Id R. (shown by points) was carried out. It is
interesting; to indicating that in Hinteregger's /2,3/
regi@trograrimes it is observed an accumulation of strong lin~;s
in the marked region. The maximum in the most extreme ultra-
violet region 60-IOG Is the most int;resting as it
corresponds to coronal highly ionized
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ion radiation. We believe, that coronal radiation variations
during eleven year cycle of solar activity, will effect
particularly the intensity and location of this maximum in the
solar extreme ultraviolet spectrum. While radiation variations
of the transition layer is mainly connected with the maximum
in the range 200-400 R.
Energy o ieW1in`( =50 R of
radiation energy of all the theoretical lines. ? -
the same according to \,\=10 averaging
according to ttA =50 R of the reliably identified
lines, presented in Table I.
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t T0pn TyPC
~ 1 g l
."'~:1 .t~.t++, .?~ rc? -,lt1"r!w~ :`,C?v~' "1.1'?rt. t'7.,j .): ~, .` ~
.1. 3.. ".c .txt?"r^f"f'!`.?^a 11,?3 :~~+~?Mt ;. u.t 7,~n;1tt 1 ' ;:f?
4, ~ i?' ?'I.'~.21.tJ?1 J.C1Gtt~;1'~ayr7.? Ox1. p, ; , P3 =7,1) .' i.
>. C. P a ', '. r ?1i+ lt, L'. "??';4>',. ;" "~'t? oc i. , Lt e 4 5, 161.
b? 8. n-Mblr , in "~ t1 CiC n. ad? $g t.I191er, ?!,I11.
n? VI.
7. .,1ctt t* , ,1v. ~;e,X~t -m., "I.
a ~~rolr,
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;j r:l c3)4; u 3: ac II t i Icat1.oi ij
A [21 Z [?] )13 r4 C3~ ] io
1 2 3 4 5 6 7 ,1
62 ,j.01 1:".! :IV a9.6 ti.lJ
.3 VLrI 61.6 U.Jtiai
i!3 ItI ~~ (G3) o. !,yJ~
ti U. 0 .1; 'Vx (67) 04 (;.-4
G9 0 1 Li VI'Ll G). a' x0.32
74 01`, ro X3,.1 (75). 0.w)
:33.9 30 33 0. f, 1,o Y.II C1$ U.06
93 0.015 110 X (9,5) 0.05
10.7 2a .t'o IX C. W03
1Jj1~J 20
It .C. a 5 111 4,05 V.L 111.3 0001
113.6 20
13.5.6 5 0 VI I.. c3 0. Uu5
..3.9 10 120 t3? ;i;;i ,3S V Ii?.) 0.01
132 0.0J4 3 c V-111 130.9 0.01
0 VI 132.3 0.005
13;33.5 15 133 0. U. e Of' VI 13.3. G u. t:;h>a
I;J.3 10 1149 0.J,;?3 0 141 150.1 00 i)15
IG:i u?Dt A K 4T. 'r) JO U15
4?
169.'3 15 169 0.u3 A X (171) ur:I'ace roc:l; i.enssiy goals
,5 ? ~~'~ (g)
c;r th raa1 p~
jL. iietc;rminatiorl of
from
In accurate value of the co "tc.'' e it cols?ioini;nt of
tcnlp;.:raturo r,ovaaleoi the lit t?ir1 into account
the i-)rob,,-iblo value: of I acco1".,in" to :ra.lc?r refi :c -
tion and rn tl0 emission data to !ete.'ii1111e the constant
component of o. real temeeor.ature To in the centre of
the hater disk ,iith an accuracy not lc.;s than -+- 5 %''? At
the same time from the calculation of the moon surface
tli.:i:nal r ,i.me the :L'o.;actions To (r), T, (r) To/Ti , T night
have boon found when
changes within 20 Y I2r)n.
To
I'he;n they eol;?pari,aon of th c~~~~eri.r.u :r~tal ?rna[alitu~les of
and To'T1 and the calculated onus : ho.;eu that the
Tatters a: ell in e rcolncilt at ti a (WPC) +I2
[IlA
which equals in absolute units
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(?350?75 (9)
ronl 3 , and coils id rinc that C = 092 we obtained accor-
,;ing; to (fl) th thermal conductivity of layer rocks
k ^' (it 0,5) ?i0-4 cat. jrnd.' cM-'sec_'
i'lli? value is nearly two orders more than the accepted
before. iippare.nUly such a hijh thacmal conductivity does
was
clot correspond to the lust in vacuo as it UGGestod ear -
her but rather to a porous material like a puanice.
)tensity and structure .LU V e-cmillation of el la (:r
rocks from thea.'ma1 c1 aIlli "tea'~3.
It has been shown above that ( itself reveals
the po,sibility to discover the lunar rock density. The
new method (15] of de tc rminin~: the lunar outer layer
rocks density is based on using; the dependence of the
thermal conductivity k(p~ on the density which
is a universal func Lion for earth rocke or . at lca;_;t a uz
"rou.p of the-A. J'llus it appears that 112
ra kpc) _ Lk (p)PCI C /
depenus only on and is a known function for earth
rocks. ince lunar rock chemical composition is like can
e artb4 one then having; r for lunar rocks we can find
Yet it seemo that the functions W (p) are different
for foamy and dry substances. For the loamy ones we obtain
P = n,4 9.c111-3
For dry ones
p O, ,. cin
L'he 1 ~t p cor"c esponii to dielectric constant E-1,5
ann the 2d to 2. Tl1e Ist value i s nearer to the
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obtJ.l'!G.i 'J 'U 1. le 1Y'. Lio s:LLt_? 1011 .:eta , hence l loamy SLruc-
tU_l' Lo the reality.
6. j)ie1ectric lropurtics of su_'2acc. later r.iat rial.
_ineralo -?ical _ _Lruc~tul'c:.
T 1 col^r. esjpon aline v~?ith tl~e knovnl eiicrl;lal paraiiotors from
the ual~re lion (1) an effective ,:electrical conductivity or
a loss-aI1L;Le tan!i;unt can be duturi,11.ned for a given wave; -
1c.n, th. the c;.eturmirlia of thc: lo.,.s-an_le tallh ant is of a
41
special inLurest for identifying lunar rocks with ith ea t1i'Sone~.
It L3 known that it c'na.ractcrizes the l,-in d of a rock, its
chemical composition. hut it also cicPunds on the Onsity, e.l.
Tllat' rlal poros t j . The comparison must be cL?rrieS out with
an electrical parameter invariable of the Jeasity. 'Iuch a
parameter is a ratio of a loss-angle tan Gent to the density
alp maC~;netudL> at is et :rminc d by only a
c1lcLlic.,1 co:n;,o3.1_tioll or a type of rock material. 1 ccordin[;
4
to (I) the invariant for lunar ruck .;
X0.6 Cr 125 ?10.6 350 - 5.10.3 9r'?' CM3
'or seerchinh ti.~,c e irth rock s sir,silav to lunar once by the
value of this Para:etcr a 1111I11erous laburator, I: eaaurei,IQ11t8
of the inva is it at VhF have been carried out for treat
earth rocks 116J . It turned out thatjo~p = 5,10
is inherent in such rocks as (L;abbro, iolitc, diabase
-"~ drani.te
(basic rocks), , rite, i_ioritc (:lidd:le >'