INFORMATION ON SOVIET BLOC INTERNATIONAL GEOPHYSICAL COOPERATION - 1959

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• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP82-00141R000200740001-1
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 28
• Document Creation Date: November 9, 2016
• Document Release Date: February 11, 1999
• Sequence Number: 1
• Publication Date: July 9, 1959
• Content Type: REPORT

1959
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:GEOPMYSI CRL ': YEAR; ; I NFQRMRT I QN
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PB 131632-73
INFORMATION ON SOVIET BLOC INTERNATIONAL GEOPHYSICAL COOPERATION
July 3. 1959
U. S. DEPARTMENT OF COMMERCE
Office of Technical Services
Washington 25, D. C.
Published Weekly
Subscription Price $1200 for the Series
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INTERNATIONAL GEOPHYSICAL COOPERATION PROGRAM --
SOVIET-BLOC ACTIVITIES
rt ble of Contcnta
Page
I.
General
1
IT.
Rockets and Artificial Earth Satellites
1
..
III.
Upper Atmosphere
16
S
IV.
Meteorology
18
V.
Arctic and Antarctic
23
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Ast::onautics Commission Created in Czechoslovakia
According to an article in the No 4, April 1959 issue (p 232) of Veda
a Zivot, published in Prague, attributed to the Bulletin CSAV (Bulletin of
the Czechoslovak Academy of Sciences), the presidium of the Czechoslovak
Academy of Sciences has established an astronautics commission in its tech-
nical section which will direct and coordinate scientific research work in
these areas, arrange scientific lectures, establish contact with similar
foreign institutions and represent Czechoslovakia in the International
Astronautical Federation. It will bring together the representatives of
individual scientific branches which have a close tie-in with astronautics.
Rudolf Pesek, a Corresponding Member of the Czechoslovak Academy of Sci-
ences, was named chairman of the commission, an its members include E.
Buchar, F. Link, F. Behounek, and J. Stransky, all corresponding members
of the academy and Docent Dr Z. Servit, Dr Engr S. Djadkov, and Dr Vl.
ICopal. The Slovak Academy of Sciences sent V. Guth, a Corresponding Mem-
ber of the Slovak Academy of Sciences, to the commission. The astronautics
commission declared that while in the foreseeable future Czechoslovakia is
not considering direct participation in launching satellites and cosmic
rockets, conditions do exist for work in relevant areas, and research.on
indirect means'should be expanded. Work will continue in the 'optical,
photographic, and radio observation of satellites and other cosmic bodies,
and the methods will be gradually perfected. Upper atmosphere research,
assisted by observation of meteor trails and research on meteor dust fall
which is well organized in Czechoslovakia according to the article, are
closely connected. Work has started in planetary astronomy with, e.g.,
study of atmospheric and other conditions on the Moon and Venus. Theoret-
ical and experimental work is being done on research di ?ected toward the
development of rocket motors. Further, theoretical and experimental work
will continue on chemical fuels research and biological areas research.
The commission's area of activity also includes the legal aspects of rul-
ing cosmic space. (Prague, Veda a Zivot, No 4, Apr 59, p 232)
Soviet Techniques for Satellite Observations Dec..cribed
A complete translation of a recent journal article follows:
Artificial Earth satellites have become permanently established. in our
lives. Very few realize, however, that the artificial satellite is a rather
unusual cosmic object from the -viewpoint of astronomy and that observation
and study of its motion has raised many new problems.
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First of ally the Earth's atmosphere exerts a very strong influence
on the motion of artificial. satellites, as distinguished from ordinary
heavenly bodies. For a considerable portion of 'their orbit, in the
region of the perigee, satellites pass within the limits of the Earth's
atmosphere to various levels, experiencing thereby a deceleration. The
effect of the Earth's atmosphere is different at different points in the
orbit. It varies very irregularly and is not yet subject to exact analyt-
ical calculation. This means that the ordinary methods of celestial me-
chanics are applicable in calculating the orbits of such a satellite only
in the first approximation.. In other words, 'there does not yet exist an
exact theory of the motion of Earth satellites which are intended for use
in solving geophysical problems. Such a theory can be developed only after
the most difficult geophysical problem has been completely solved, namely,
thorough investigation of the Earth's atmosphere.
Since there is no analytical theory of the motion of satellites, it
is impossible to give exact predictions of their position over extended
periods of time. The motion can be predicted only for several days, since
such predictions must be constantly corrected on the basis of observations.
The method consists of calculating a certain average orbit for the geophys-
ical satellite and improving the elliptical elements of the orbit and their
secular variations on the basis of observations over 10 to 20 days. It is
very essential here that the observations on which the improvements are
based be taken over as large a segment of the satellite's orbit as possible
From the viewpoint of astronomy, this indicates that it is essential to
conduct regular observations at various points on the globe and to transmit
the results of these observations to a computing center in as short a time
as possible.
In conjunction with the program of the IGY, there was organized a net-
work of special observation stations, puking in almost all countries, the
unique "satellite service." Chiefly, visible observations were conducted
at these stations, using wide-angle astronomical "satellite" telescopes.
Visual observations do not require specially trained observers and do not
need extensive processing. Within an hour after the observation, the re-
sults can be transmitted to a computing center and used to calculate the
motion of the satellite. This makes visual observations extremely valuable
for a short-run service, although they do not have great accuracy. From
the moment the First Soviet satellite was launched on 4 October 1957, 70
visual stations were continuously operating:in the USSR, more than 100 sta-
tions of the "Moon Watch" system in the US, 59 stations in Japan, 18 in
the Netherlands, 14 in China, 13 in Czechoslovakia, 10 in Poland, and 8 in
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East Germany. At almost all station, the observations were made enthusias-
tically by volunteers, including students, acicntifie workers, amateur
a;;tronomcra, and school children. By 1 January 1959, the computing center
of tiie USSR had received data from more than 11.2,000 observations on the
first, second, and third Soviet satellites; of these 17,000 were from 35
foreign countries. Information on their observations is regularly received
from stations in Czechoslovakia, China, Poland, Holland, and Japan and from
observatories in Finland, France, South America, Australia, and East
Germany .
The AT-1 telescope is used to make observations in the USSR. These
telescopes are mounted on tripods or bench-stands. The AT-1 consists of
a small wide-angle telescope with an entrance-pupil of 50 millimeters, a
magnification of six, and a visual field of about 11 degrees. In the
visual field, there is a system of rings at one-degree intervals and cross-
hairs marked off in 20 degrees of arc. To insure sighting the satellite
which has a low luminosity and moves through the sky with a velocity of
one degree per second, when its orbit is known only approximately and even
sometimes completely unknown, one or two "optical barriers" are organized
at the stations. These consist of 20 or fewer telescopes, depending on
the accuracy of the preliminary ephemeris of the satellite. The barriers
are placed along a meridian and along a vertical circle perpendicular to
the visible orbit of the satellite.
To determine the moment of passing, with an accuracy exceeding one
second, the stations use a printing chronograph. The null-point is deter-
mined from an exact time signal transmitted by radio. The coordinates of
the satellite are determined from star maps.
Experience in the stations has shown that the majority of the observa-
tions determine the position of the satellite with an accuracy of up to one
degree. The dete.ination of the moment of passage is much less accurate
and is given within fractions of a second only at the best stations. Ex-
cluding clearly erroneous results, (such as when meteors or the exhaust
from an aircraft is taken for the satellite, the section of the sky in
which the satellite was observed is incorrectly identified, or the time
signals were read incorrectly,) the average departure of the observations
from the computed orbit was within one or two degrees of the right ascension
and declination. A systematic analysis of the quality of the observations
began in December 1957, when a group of scientific workers of the Institute
of Theoretical Astronomy undertook the task. Since Feb-uuary 1958, special
bulletins have been distributed to the stations indicating the departures
of individual observations from the computed orbit. Six issues have al-
ready been distributed, in which appeared the results of observations on
the second satellite and the rocket of the third satellite. Three more
issues are in process.
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After the launching of the first US satellites, our stations were
prepared fccr observations. Ephemerides which arrived from `the US were
regularly obtained by the southern stations. Unfortunately, we were never
once successful in observinG even one of the first three US satellites.
Although optical barriers were set up in such a manner as to "intercept"
them, even if very low over the horizon, the brightness of these satellites
was too weak for observations from our latitudes. The inclination of their
orbits to the plane of the Earth's equator was less than 34 !degrees and
they did not pass over the territory of the USSR. Conditions for observing
the fourth US satellite in 1958, which was also* weak in brightness and whose
orbit had an inclination of 50 degrees, were for a long time unfavorable
and only in December of 1958 did the first observations begin to come in.
In the succeeding half year, apparatus and observation methods were
considerably improved. For example, a simple sight designed by B. E.
Tum.nyan (Yerevan) and attached to the AT-1 Telescope facilitates finding
the object and identifying the section of the sky, and helps the observers
to check their work'. The site consists of a ring, two rods, and two diop-
ters and can be made at the stations.
In the northern regions of the country, a considerable portion of the
observations was made during the early evening, when it is difficult to
determine the position of the satellite; in the visual field of the tele-
scope, there are either no stars visible, or only a small number of stars.
In this situation, theodolytes were used in certain stations to observe
the satellites in the azimuthal system of coordinates without directly con-
necting it to the stars. Since the visual field of a theodolyte is very
small, AT-1 telescopes were mounted on .he theodolyte stands at Khabarovsk,
Kzyl-Orda, and Tartu. Such an installation retains all the qualities of a
theodolyte and, in addition, offers the . arge victual field of the AT-1 tele-
scope. On this basis, Ya. R. Eynasto of Tei;u prepared an experimental,
automatically recording theodolyte. Attached to the body of the theodolyte
iu a photographic device which takes a picture of the readings of both
circles of the theodolyte through a microscope; up to 20 positions over the
whole visible trajectory of the satellite can be obtained. A careful in-
vestigation of satellite observation methods for use with theodolytes was
ccrducted at the station under the Pulkovskiy Observatory (D. Ye. Shcheglev)
and exposed possible sources of error.
Finnish astronomers provided valuable results of their observations
on Soviet satellites in the azimuthal system of coordinates. In addition
to visual observations, many stations took photographs of satellites with
small cameras of the "Tfkiyev" or "Zorkiy" type. The beginning and end of
the exposure was timed with stop watches; chronographs, or magnetophones
or tape-recorders.
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To be sure of photographing the satellites with the sma.ii cameras, the
Yuzhno-Sakhalinsk (K. N. Kun) used the AT-l tcle,dcope as a telescopic view-
finder. The photographic equipment was installed pax-a,11' 1 to the axis of
the telescope. The ax:Lo of the objective of the photogrcp'r?.ic equipment
forms an angle of 45 degrees with the plane of the `:eleccope mirror, as
does the axis of the AT-1 telescope itself. This makes it possible to see
the object simultaneously in the visual field of the telescope and in the
viewfinder of the photographic equipment and positively to locate the ob-
ject in the sky and photograph it. On 1 January 1959, the cameras were
used to obtain 23 pictures of the ru.:ket-carrier of the first satellite,
192 pictures of the second satellite, 342 pictures of the rocket-carrier
of the third satellite, and 10 photographs of the third satellite, Photo-
graphing the third satellite with the small cameras p -esented an extremely
complex problem, since its brightness varied greatly, and it was seldom
visible to the naked eye. Considerable success in this respect, was had by
the observation station under the Vologodsk Pedalog:LcalInstitute (A. P.
Pole-ta,yev). During February 1959 alone, this station obtained. 6 photo-
graphs of the third satellite.
Exact photographic observations are necessary to solve scientific
problems connected with investigation the Earth's atmosphere, the shape
of the Earth, and geodesical problems. (Footnote:) It is interesting to
note on the basis of 47 observations of the second Soviet satellite (chiefly
visual), which were made from 5 November 1957 through. 21 March 1.959 at the
stations in Czechoslovakia, Czechoslovak scientist E. Bulx_bA: determined the
position of the ascending node of the orbit of the satellite and calculatled
the coefficients of dynamic contractions K and the cont:action of the Earth,
2. as K = 0.0010852 ? 0.0000013 and o` = 1/297.90 ? 0.18 (Siuaia - Geo-
physica et Geodaetica 2, 306, 1958).
On the basis of the photographs of the track of the :satellite among
the stars, it is possible to determine very ac?rzrately the position of the
satellite in the sky. in photographing satellites, astronomers came up
against another new problem. The satellite moves through the sky relatively
rapidly, on the average of one degree per second. This means that if we
wish to determine the position of the satellite with an accuracy to one
minute of arc, then the time of the passing of the satellite must be deter-
mined with an accuracy of approximately 0.01 second. Fo: accuracy in the
coordinates to one second of arc, the time reading must be accurate to within
0.002 seconds. Consequently, photographic observations must be made with
an astronomical telescope which has special provision foz er act time
measurements. The existing large astronomical telescopes in the observa-
tories have not until now needed such very exact "time" capabilities since
the motion of ordinary heavenly bodies is extremely si.ow. New instruments
and modifications on existing instruments would be needed to photograph
satellites. In the US, special wide-angle telescopes of the Baker-Nunn
type were constructed for this purpose with a diameter of 50 cen,imeters.
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A quartz clock attached to these makes it possible to determine the time
of passing of the satellite to an accuracy of thousandths of a second.
These cameras have high optical properties, which make it possible to
photograph the very weak American satellites. Twelve such cameras are
operating at present and are situated along the equatorial belt. Photo-
graphs obtained in these are sent to the Smithsonian Observatory in Cam-
bridge, which is the co-ordinating center for all optical observations
in the US. Here, the photographs are measured, using a single method,
and the results are analyzed. Asa result of the high optical qualities
of the Baker-Nunn camera, th? second US satellite (1958,8 ),which is a
sphere of a diameter of 15 centimeters, was successfully photographed on
10 January 1959 in New Mexico at a distance of more than 600 kilometers.
In the USSR, NAFA-3c/25 wide angle aerial-photography cameras are
used to photograph satellites. These have uran-9 objectives with a 25-
centimeter focal length, 10-centimeter objective, ands visual field of 32 degrees
by 52 degrees. Using highly sensitive film (1,100 units according to the
national Soviet standard for aerial photographs), such a camera can photo-
graph an object of the third stellar magnitude moving with a velocity of
one degree per second. A receiver, a pulse output unit, and a printing
chronograph are used to denote the exact time.
Before the satellite passes, the camera is aimed at the required sec-
tion of the sky; then, the observer, using a pocket viewfinder for the AT-1
telescope, after he is satisfied that the satellite has entered the visual
field of the camera, opens the shutter several times for short time inter-
vals. Special contacts installed in the shutter mechanism send signals
which are recorded on the chronograph tape at the instant the shutter opens
and closes. Time signals transmitted by radio are recorded on the same
tape. The rhythmic time signals transmitted from the time services of the
observatories may also be used. Specially constructed pulse outputs have
been installed in stations not having their own time service so that time
signals might be recorded on the tape of the printing chronograph.
The position of a satellite on the photographs, taking into considera-
tion the complexity of dpterminging the exact time of exposure can be deter-
mined with an accuracy up to one minute of arc. The final stage of photo-
F,-aph analysis is done on special measuring instruments, using ordinary
astronomical methods. The majority of stations used the method of A. N.
Deych and A. A. Kiselev (Pulkovo) to determine the position of satellites.
The method is based on interpolating the equatorial coordinates of two
reference stars situated on different sides of the track of the satellite
or rocket to the point of intersection of the line connecting these stars
with the track. The results of the exact analysis were made public in the
bulletin of the Optical Observation Stations for Artificial Satellites,
published by the Astronomical Council. By 1 January 1959, the 26 stations
for photographic observations with the NAFA-3C camera had obtained 7.6
photographs of the rocket carrier of the first satellite, 265 photographs
of the second satellite, 82 photographs of the third satellite, and 1,,524
photographs of the rocket carrier of the third satellite.
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Even more exact coordiria.tes of the satellites could be obtained by
adding to the large astronomical telescopes a special device which would
insure the exact recording of the time of exposure. The first such equip-
me,it was made at the Astrophysical Institute of the Academy of Sciences
Kazakh SSR.
A special adaptation to the telescopes was developed at the Astro-
nomical Observatory imeni Engel'gardt, close to Kazan. This makes it pos-
sible to record the times of passage through certain points on the photo-
graphic plate. A plane parallel glass plate is placed it front of the
photographic plate. The glass plate is marked with a network of parallel
lines. The frame of the plate turns relative to the photographic plate
during the time of exposure. The position of the lines of the grid is
then recorded at certain times on the photographic plate. A pulse illum-
inator is used to produce the 1ni tges .
The velocity of the plate is selected in such manner. that it moves
through 20-30 millimeters during the time ofexposure. There are dis-
continuities in the track of the satellite on the photographic plate where
the image of the satellite crosses the lines of the network. The times of
these discontinuities are determined by measuring their positions and the
positions of the lines at the fixed times at which the illuminator operates.
An analagous method of photographing satellites was developed by Ye. Ya.
Bugoslavskaya at the Astronomical Institute imeni Ste:^nbewg (Moscow.)
A method was developed at the same institute for photographing weak
satellites, using electron optical converters. The idea of using such con-
verters and thus considerably increasing the sensitivity of the instrument,
was extremely far-sighted. However, there is no real gain from using them
unless the object is observed against a dark background. Since the exist-
ing satellites are observed only against a twilight background, this dif-
ficulty has unfortunately not yet been circumvented and no photograph of
the relatively weak third satellite has yet been obtained.
At the main astronomical observatory (Pulkovo), a c,me::a with'a moving
film was constructed which makes it possible to record satellites which are
weaker than can be photographed by ordinary methods (I,. A. Panayotov).
This interesting method was proposed by M. K. Abele, a scientist at
the Rizhskaya Station. The satellite is photographed on an oscillating
plate through a telescope. The direction of the line :long which the photo-
graph plate oscillates, coincides with the direction of motion of the satel-
lite. As a result the track of the satellite obtrine, on the plate is not
in the form of a streak but in the form of individual points at which images
of the satellite are superimposed, one on the other. This method makes it
possible to photograph the weaker satellites. The moment of the individual
exposures is recorded with an accuracy of within 0.001 sec=Ls.
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Soviet satellites are regularly photographed abroad. By 1 January,
3b photographs of the rocket carrier of the first satellite had been ob-
tained, 272 of the second satellite, 1,800 of the rocket carrier of the
third satellite, and 270 of the third satellite. The great majority of
the latter were obtained on Balser-Nunn cameras in the US.
Good photographs of the satellites were taken by astronomers of the
Potsdam observatory (East Germany). The German astronomers sent a fortu-
nate photograph on which was caught the track of the rocket carrier of the
third satellite and the track of the US satellite 1956 c [Explorer 41.
The photocraph points up the relative brightness of these objects.
Study of the change in brightness of artificial satellites presents
interesting problems. The visible brightness depends on the change in the
phase of the satellite, i.e., the fraction of its visible surface irradiated
by the Sun, on the change in the distance to the observer, on the absorp-
tion of light in the segment of the path from the satellite to the observer,
on the rotation and tumbling of the-satellite, and on the change In the
state of its surface. Large-scale observations with subsequent statistical
analysis are required to obtain useful results.. Visual photographic and
photoelectric methods may be used for such observations.
The photographing _'.s done with still cameras. The brightness of the
satellite is determined by comparing its track with the track of the sur-
rounding stars. The difference in the velocities of the satellite and the
stars must be taken into consideration, as must the dependence of the
sensitivity of the photographic-emulsion on exposure time. Because of the
difficulties of accounting for these factors, the photographic method re-
cults in an error to several hundredths of a stellar magnetude. Analysis
is made easier if the photometric error of the field is known. The Picker"
in,-method used in observing variable stars is used to estimate the bright-
ness of a satellite in comparison with the brightness of stars situated
along its path. The brightness of the object is given in tenths of the
brightness of the stars to which it is compared. In satellite observations,
such an estimate must (kie made over 2 to 3 seconds . Since mid-March, about
50 visual stations have been engaged in these observations. Analysis of
the observations obtained at various points on the ED th is being done at
the Odessa Observatory. Also being developed is a method for determining
the position of the axis of rotation of the satellite in space.
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Even during observations on the rocket car, :r of the first Soviet
satellite, the attention of many observers was urawn to the very obvious
oscillations in brightness. The chief reason for these oscillations is
the rotation of the rocket around its transverse axis. he amplitude of
this change, according to calculations of Japanese observers, is 5 to 6
stellar magnitudes. Even more considerable was the amplitude of the change
in brightness of the Soviet satellite (6 to 8 stellar magnitudes). An
analysis of the large number of observations permitted V. P. Tsese?iich
(Odessa) to determine the average period of rotation of the satellite
around its axis. This was found to equal 208.5 seconds. He was also able
to show that during the lifetime of the satellite, this period changed
from 180 to 230 seconds,
An interesting feature of the rocket of the third satellite was the
periodic, comparatively short-tern, oscillations in brightness caused by
tumbling around the transverse axis. Photoelectric measurements made by
J. Moore (California) showed that the period of the oscillations in bright-
ness changed from 15 seconds in the beginning of June 1958 to 18.4 seconds
in the middle of October 1958. Analagous results on the basis of a large
number of visual observations were obtained by M. S. Zverev and M. I.'
Yesipova (Pulkovo). The third satellite itself, as a result of its shape
and high altitude of the Earth, was rarely visible to the naked eye. .Out-
side of individual instances when a rather smooth rise and fall in its
brightness could be observed for the course of 50-60 seconds; there was
more characteristically an instantaneous flash with a very rapid and sharp
drop-off. Evidently we have here simply a flash from some narrow reflect-
ing portion of the surface, By 1 January 1959, 48 stations had obtained
about 200 estimates of the brightness of the third satellite, which is
clearly inadequate for drawing any conclusions concerning its rotation.
The study of the motion of artificial Earth satellites is a large and
important international task. The results of the observations on the motion
of satellites convincingly shows how great is the striving of scientists
for ess-like co eration and what a eat advantage it can brio to
C PYRG H ci a e Astronomical Observations on Artificial Earth Satellites, by
A. G. MWsevicih, Doctor or 2hysicomathematical Sciences; Moscow., Vestnik
Akadeemii Nau:c, No 5, May 59, PP 85-94)
Special Telescope Devised for Satellite Observations
The following article appeared in a recent Soviet journal:
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Q. for p.hotogi?aphir., onse:?vation:~ on F .;;?th oate1-
;?r) 67 in the ref' ,York of ?31milar stations in the .3oviet Union, was
sF up in Or;tc`:e:_ 1957 by the As';:^ophysioc.l In ;it?:te of the Academy of
S.::ienc:e ?tnzra.kt: SSR on the iC nen.;koye Plateau nsar. A!=:-Ata. 7ae station's
equipment aonsiots of a 'wife angle "Soxfi'r" Boyye C;:nre:: ,, (100-millimeter
ob.jc ,give and 45O-m.:Llhitrveter.' focal length) an? a 6 hall cwiiera with a
`:Z,O.r17:LI? objective. A s. top inox'ated. in front of the objectives ps od.u~:es
bra,,k;: !A. ,tie image of t.":se rY.+~lli' e `t'ack at r ''ne:" irt7.R.-r-Led by as
o':? y ch onograph an xr.k::s it possible to .:y>L1~:hror.ise the motion of
the ..a,;~llite wi'',h the C'r_ro.r nk:t~ rnaiiing,3. E-!uip.,n t which make it
to ~'eterinine the ^-.onn inat-,es with an a::curacy of one minute of
ar., an:'. to z? ,c', a fi.2ue *vi hh an ac:'urac of up t O.O , se '?on~.
Y was su :cesF-
fully applied on 23 Oat~obe:c 1957, when the rocket, carrier with the first
Soviet artificial Earth satellite rose from behirt1 the mowntainr? of Zailiy-
skiy /!1N.-?Tau for 'rre fi.r?s';, time ielot, otc? 1ati4;uC .
1911-, ~,{,Jipment;, of :::tr:s? c;~.: t be calli!O. f'i:.Ot either with
y-,.-..-6. to tH-:~ n.ou_?.a.y of photographic: ?_t; try ina?tioni-i o:.^ frith :regard
to the p,:n,.t:?at1ng pave-_-, -? .e., 'r.?-i,:i o,'5ility t^ cot,31 .ices vi-";h
lnw ill Lie.1-icn Th? of f'o`? ;s of the u-er'~ th_ e=efre
impss Jving mr''.:hor_:; of phot;ograp't.ir..g, p;..'i1>viw'il.y by raising
t.ho: sen.s i;.,ivity of tl?.e? ,,mall - am~~ caa to the rac.N:-k.:; waz:~k satellites.
Ai_. it ii cv sky., the leave:. N more
c"- .L?~:;. C.IE.':,ire: ::Ic :-)n p1'.o'i;og epf:.. .J1 ?r;'"n=; f '_."?ot appro..Am .'bion, the
ei e: t of i's a.'*::Icn or. 9. p^o log 'aphis emO_sion i_...:~?~'?_i~rz wit:;a an increase
in t..b.e '. a1ue
v.
In ;he: p:'0-9.e a 1u _7; L' 7s a.1e C'i?_.TM1t:.j:?' c:.' ,:r~iT1N "a objective, F is
the f cca? y i, eg'c!1 of the tit jeer ;a.'v ~ , v is -the n linen.: 'wile::,, y of the moving
i g,-' or. i i (.'. z, fY.O _ of. -.e e : u2,iicn, a . Q iz t1e, fJ.rumC-": ter of the sc:at'?
te::?i ng i. .e . , th" o ne? by the o".:' js ;ive of a stataionary
point o:? light, at. an infini ist=ce. Wi?,,ho'. , going into c'.etail_, it may
ba :?a .c' t;rat photog7raphi:. int. nand for :'c_?- ving a:. tific:ial Eazth
inuet :-oir. ine prcpt:'~~ies uhir_??a hig... anc' yet very difficult
to coo: ?-cli a e 'with one an_c t;he~? from the viewapoi n- of optica1 ehbez'atiuns.
'l lP.:;?~ t1:... :7. db jac live ?1=e ter, a :Age focaI 'length
of i.:.'tezn Lni n,g the C~:C::':.1 n::';? J i? ?~:.?i'.' ~3r s a-IL 'o G
'.i onF'.:...i _ - z.,th.e of a , s~ . a1' _ z. ..`,?c Fur face . ?r.:.li:.c ,')~ , .~r...ii..g ace Fi'fi pas-
s ible' and a large at gu.Ic.?.' 'f'ief:.. In ~1 ?._ it ::t y 6*tsert'ati on p 'actice,
we :: -_r aak only of :'_ao:rn Lrg t~e phoi:ograF'-i : rac>:i.> c5 vil l be =_ali-zble from flying labo-rz.toriea3 ancl a7~-U-
f:
7 t o:i the ] nimea i. . i, pr:.ab.icros in the de-re? opmen?+; of coamonauti(.c is
the 1=.t :c.:.1ng of an- ~.n%-x "Ianei;a::y craft which will fly a::ours. the . Moon
at Ai Mane..,, t:1 it a a , will repox,? f.e ailed i `?i.'o:: L` do:b Coi:-
C. f? i a ~pc::'! to J wi S of the 1' i jra c anCl lire
pL y,,'l:ses~ eo . ?.i;?orv o came .-:.s e^n.f' othe:. c'~Lrpi e7-L"eip1!ic it
iz.ig ir'e::esting da?.t;a. .onza2 i'ng aeatain p.acv:Lia :?i-
ie o:' a a in roJ_'t iv i,
{ _ ...Llrx?. tir0:: ~ r:. must -Oe E ;~t;f;blis_ed ii.. .._.( .C' C C . M, ..E; -.i.:a''lOrl
c: a' . :;e.tcc;flit,:: of, he Moot, (whic`. is also sc e.?.u2 e will eon-
~, a t ~ :7 n..,:. t a i e11 !t. t ,rt. o to fly . it. ~ra~:bly .~Icay Its ?.c:?':.a:,..~: Study. dy. _~'X' s~t .., R.a;,c ~ 'x?,. at,
R:,.,~li..
:?Ln alt j %-lu .(: :F ;0 kil' eto, o; fin the lun1:.. even dc'= 1.ia
of 6. meter;; can be teen f:.-am i?{,. -t is t.'.-11c
the must move with a ay'a.~( c? of more tip-, 1,600 mcte_?=; per second
aa?~. 1;;~?.'? or 1=P objects 1:e1.L'g obse_Jed will be quickly !not late.,- than
6.4 I:.'].l'xi;-L3 tr i on fie'l: c view of the iri t2"ments (:a::,iec. in the
Anr. '_11'. 150 kilometers., lr.h.c` na:;,:L:L= t ti-me any object
will b to 15.7 minutes, wh: !.e the size of object
must be t'Ze nrl.kecs eyv , no _ess than 31-5 Mete.%a .
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The launching of an artificial satellite of the Moon would also pro-
vide very great returns on the score of investigations of the physical
parameters in the neighborhood'of the Moon: the magnetic field, the in-
tensity of the cosmic radiation, etc.
The next stage will be to launch an interplanetary rocket, with the
aini not only of flying around the Moon, but also of landing on its surface.
Then, scientists will obtain such information as is impossible to report
from flying cosmic craft. Apparatus landing on the moon can measure the
temperature of the lunar soil at various depths directly, give more accu-
rate information on the structure of small portions of its surface, on
the properties of matter forming its surface layers, on the density and
composition of the rarefied lunar atmosphere, etc. All of this is a very
important link in the preparation for cosmic flights, with the participa-
tion of people themselves.
Flights by man in interplanetary craft will lead to new, extremely
interesting, discoveries. The launching of artificial Earth satellites
and the first cosmic rocket showed that man's escape into the cosmos is
fully possible. It is not impossible that the first lunar travelers will
find rock possessing new properties which may be used on Earth. With
CPYRGHT time, lunar astronomical observatories will rise. CPYRGHT CPYRGHT
"It is possible to r ose " says Barabashov, that the next stage in,
the development of cosmonau cs w be dispatching, at rs , large auto-
matic cosmic rockets, and then, obviously, also rockets with people to the
nearest planets, Venus and Mars, which will reveal all their secrets to us.
Thereafter will follow flights to the most distant planetary bodies and
finally beyond the limits other stars and 'planetary
systems." ("Artificial Earth Satellites and Problems of Cosmic Flights,"
by N. P. Barabashov, Kharkov; Moscow, Nauka i Zhizn', No 5, May 59, pp 17-
PYRGHT 19)
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S,-.)v Let S< j.:=n?ti.gt Diec~.ssc:r New Model of Upper Atmos2here
The otruc:ture of a modern model of the upper atmosphere based on
result of ra; ;n?t studies is the subject of an article by B. S. Dani? in,
Gancii.c'.;"..~ of. Technical Sciences, a summary of which is presented below.
The launching of a.rti.ficial earth satellites made it possible for
the first, time to determine the density of the atmosphere at 'great alti-
tudes. Desp.Ltc the fact the; the motion of satellites occurs in the ex-
tremely rarefied layers of the Earth's atmosphere, where the density does
not exceed a billionth part of the density of the air at ground level
and ;he force of the resis?i?,ance even in the lowest pq of the orbs: does
not e:Kccced two grams p'-.-.r square centimeter of crone section, the collisions
of the c:nteUite with the molecules and atoms of the gas cause its breaking,
leading -;he> shrinking; of its orbit and a change in itr, orbital period.
The perigees of the Soviet artificial earth satellites were at alti-
tudes of 226-228 kilometers. An analysis of their braking and the direct
of tho tiensi?ty, using manometers in Sputnik III, indicate that
the ;E.IL.e of, c'.ensity at this altitude is 3.10-13 grams per cubic centimeter.
Analyi{i.s c.f the bra:iting of the American satel.i ten, Explorer and Vangaard,
showed thit the d.enr,ity at altitudes f 368, 1+C5, and 720 kilometers con-
si~;tr:, corr . !spondingly, of 1.5 ? 1.0-1 , 9. 10-1 , and 1.2 ? lo-16 gr:.~me
per c bi.
Kno,!d.ng the change in the density with altitude, it is possible to
ds?;erm_ n,:. the so-r:a1 ed Vtaltitude of a homogeneous emosphere." The larger
the mat :'_-ular ve~ight of ttie air and the lower its temperature, the lower
the eltit'.de of the homogeneous et;mosphere. Knowing this value,, it is
?r.,o c,52.1,2u:a.?te th t=peratu_re of the upper atmosphere and. also the
r~c?eSsu-*.re end ?;o construct a modern model of the atmosphere
boxed c:t th- result,,:: of cpex-imental investigations.
c:bser-. ed braki.ngs cf sa eUites and =xomc:tri . meaBur?ments irdi-
re:tr: high 1,:.., iperatua e of the upper atmosphere -.end its considerably
den , ~r , .: uc W; high anti tL~des and Flxlly disproves eal Tier existing
o; iniou..; ;or errmirg cold end strongly rarefied upper layers of the air.
Num, , Cil;.F: obser-trat.ions of aurorae, of the change in the Earth's mag-
netic fi'-::.'i3., of twitt gh-t phenomena, of night airglow, of meteors, and
of the i.ox.osphere suggest-e i to scientists that the atmosphere expands under
heating by day and con';races under cooling at right and that in it occur
solu?: and 2'.una. tic? ~a .
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However, the experimental investigations by artificial earth satellites
and the launching of high altitude rockets (including in the polar regions)
during the IGY period alone made it possible to establish the regularity
of these phenomena. It was discovered that the diurnal summer density of
the atmosphere is almost 20 times greater than the night winter density
and that the density of the atmosphere in thF polar regions is approxi-
mately five times greater than that near the equator. It was established
that the Sun and those numerous processes which arise up on it have an
exceptionally great effect on the Earth's atmosphere. Solar radiation
and the particles ejected by the Sun are the reasons for magnetic storms,
causing aurorae and ionization of the upper layers of the atmosphere.
Strong magnetic storms are simultaneously accompanied by an increase in
the braking of a satellite which obviously is connected with an increase
in the density and, temperature of the atmosphere. ("Model of the Upper
Atmosphere)" by B. S. Danilin, Candidate of Technical Sciences; Moscow,
Nauka i Zhizn', No 5, May 59, p 20)
Unusual Finding of a Meteorite
The finding of a meteorite at the imeni M. V. Frunz placer mine in
November 195' is reported by A. I. Shul'zhenko. The mine is located in
the Susuman Rayon, Magadan Oblast.
The meteorite, which weighed 15 kilograms, was discovered by a worker
at the 31+-meter level. When broken into two parts the exposed surfaces
showed a clearly expressed crystallic structure, the crystals of which
were triangular in shape and were strictly oriented. Inclusions of mineral
matter occurred between the crystals.
The meteorite's outer surface was fused in appearance and bore the
marks of weathering. The elongated shape of the body was reminiscent of
a cobblestone. The object possessed magnetic properties.
A chemical analysis showed the following composition: 0.11-0.5 percent
carbon, 5-6 percent nickel, and the remainder iron. Other ingredients
were not detected in the fusion. The composition of the mineral interlayer
between the crystals has not been subjected to an analysis. The matter's
specific weight is 7.82.
The chemical composition and the location of the discovered body
make it possible to tentatively propose that it is crystallite of mete-
orite origin. ("Finding of a Meteorite)" by A. I. Shul'zhenko; Moscow,
Priroda, No 5, May 59,.p 115)
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V1. METEOROLOGY
Soviet Hydrometeorological Instruments Described
A description and photographs of some Soviet telemetric and automatic
hydrometeorological instruments appear in Priborostroyeniye, official
monthly scientific-technical and industrial' journal of the State Scientific-
Technical Committee of the Council of Ministers USSR. At present, says
the source, specialized plants ;manufacture up to 160 different hydro-
meteorological instruments and stations. Some of the most interesting have
been selected for presentation.
Figure one shows the remote meteorological station DMS-N-53, which
is used for quick determinations of remote air temperatures and humidities
and of the speed and direction of the wind at the level of the devices of
the respective transmitters. The station is portable and is easy to oper-
ate.
Its operation is based on the conversion of the measured meteorologi-
cal values into electrical values, which are read visually from needle
gauges on measuring instruments located at the receiving station. With
the aid of such instruments, it is possible to measure the speed of the
wind within the limits from 2 to 30 meters per second, the direction of
the wind from 0 to 360 degrees, and the temperature of the air from +4+5
to -4+5 degrees centigrade.
For complex ship conditions, the ship remote station SDS, permitting
the measurement of the mean value of the speed and direction of the wind,
the temperature and humidity of the air, and the temperature of the sur-
rounding water, has been created and placed in series production. The
station consists of a control panel and transmitter units (Figure 2 and
3). Such stations are successfully used on ships.
For operations without human intervention, under the conditions in
the Antarctic and in barely accessible, uninhabited regions, the auto-
matic rain gauge M-1+ and the automatic radiometeorological station ARMS
were created and placed in production.
The radio rain gauge makes it possible to measure atmospheric pre-
cipitations falling in liquid form and to report their quantity by radio.
Each such transmission consists of the identification signals assigned
to the given station and signals denoting the amount of precipitation.
The transmission range of the automatic rain gauge is 50 kilometers.
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The ARMS automatic meteorological station makes it possible to trans-
mit by radio, at distances up to 600 kilometers, the atmospheric pressures,
air temperature, wind direction, and the solar radiation at the moment the
station is in operation, as well as the amount of precipitation between
the periods of radio transmission.
An instrument for measuring the humidity of the soil under field
station conditions without taking soil samples for drying has beer created
(Figure 4).
The instrument's operation is based on the measurement of the degree
of reduction in the gamma rays penetrating the soil layers. The instru-
ment consists of a gamma-quanta counter, a power source, and a rod which
has a radioactive source on its lower end.
The error in the measurement of humidity by gamma ray examination of
the soil layers at 20, 50, and 100 centimeters and at a gamma level of
10,000-12,000 pulses per minute consists of t 1.5 to # 2.0 percent.
A portable snow gauge was created for measuring the water content
of snow based on 98e attenuation of gamma rays radiated by the radio-
active isotope Co .
The portable gamma snow gauge is a snow gauge having on its lower end
a steel tip with a container for isotopes, and at its upper end, a gamma-
quanta counter. The determination of the water content in snow cover is
based on. the measurement of the degree of attenuation of gamma rays radiated
by a radioactive isotope during their passage through the snow.
The instrument makes it possible to measure the water content in snow
with an error of 3-5 percent with a snow depth of 3 meters.
The automatic radio-wind gauge ARIV is a meteorological instrument
for the automatic radio transmission of information concerning the mean
velocity and direction of the wind from open'parts of water reservoirs.
A ship hydrosonde was developed for continuous, automatic registra-
tion of the vertical distribution of the temperature and salinity of sea
water in a layer of a depth of 2 to 220 meters. The bridge zero method
of measuring the resistance by direct current for pressure and temperature
and by alternating current for salinity is used in this instrument. Re-
cording is produced on uniformly-moved recording tape by --arious colored
inks.
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For measuring and recording the speed and direction of water currents
during stationary and expeditionary investigations of current systems, an
independent, photographic current recorder with a tape-feeding mechanism
was developed. The instrument is based on the principle of automatic
registration of the speed and direction of sea currents by tvvsans of photo-
graphing the readings of the tachometer of the bladed wheel and the com-
pass.
Airplane dropsondes intended for measurement of the pressure, tempera-
ture, and humidity of the air from an altitude of 15,000 meters down to
the earth's surface parachute descent from the weather are being built.
The results of the measurement of the meteorological elements are trans-
mitted by the sonde's radio transmitter in the form of.telegraphic signals
and are received by the plane's radio-operator or recorded by magnetic
recorder.
For measuring the relative humidity of the air under ground conditions,
a hygrograph using animal membrane as a transducer was developed and is
manufactured (Figure 5).
For measuring the humidity of the soil under field conditions, with
a temperature over zero degrees centigrade, the AM-11 soil humidity gauge
was developed and manufactured (Figure 6).
Automatic recordings of the temperature distribution in the layer of
water of'a depth down to 200 meters is ensured b a thermobathygraph, being
manufactured at the present time (Figure 7 and 8)).
Photoelectric cloud meters, parachute-dropped from a weather plane
from 15,000 meters, are proposed for determining the upper and lower
limits of cloudiness for middle and lower strata. Upon the entry of the
instrument into the cloud, a scattering (by the cloud) of the light being
radiated by a pulsed source occurs, as a result of which the light pulses
fall on the photoelectric cell and are converted into electrical pulses.
The mangnified electrical pulses enter a manipulator controlling the radio
transmitter.
The registration of icing is of great value to scientific investiga-
tions and to maintenance operations for railroad transportation and for
telegraph and power transmission lines. For determIxng the weight, inten-
sity.,type, form, and dimensions of icing on wiring, the M-28 icing meter
was developed. At present, the Scientific Research Institute of Hydro-
meteorological Instrument Building was developed a remote icing meter.
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This, says the author of the article, is not a complete list of all
of the products of the new technology created by the scientific research
..n;:;r,itutions of the Hydrometeorological Service and the products already
;,,:sinj3 developed and produced by specialized plants.
At present, major work is being conducted on lowering the cost of
instruments being produced by the introduction of an efficient production
technology in machine and bench operations, the introduction of conveyor
lines for the assembly of instruments, and the mechanization and automa-
tion of laborious check operations. The role of plant laboratories in
the solution of production and research problem is continually increasing.
The work of the central plant laboratory of the Rizhskiy Hydrometeorologi-
ca:1 Instrument Plant is a good example in this regard. Direct contact
with production is extremely important for plant laboratories.
Along with the suc,.~ssses achieved in the field of hydrometeorologi-
cal instrument building and in the work of creating new and perfecting
existing hydrometeorological instruments, there are shortcomings. The
most substantial of these still is the significant lag in the develop-
ment of mass-produced instruments which are necessary for increasing the
accuracy of observations, lightening the work load of the observer and,
in many instances, replacing him. Another, is the absence of automation
in the processing of observations.
It"is necessary to more intensively design and introduce mass-
produced. hydrometeorological instruments utilizing the means of tele-
mechanics, radio electronics, and other modern achievements of science and
engineering. ("Hydrometeorological Instrument Building," by A. B. Reyfer;
Moscow) Priborostroyeniye, No 4, Apr 59, pp 26-28)
Re-evaluation of Book on I.ong-Range Weather Forecasting Urged
Although B. P. Mul'tanovskiy's book, Osnovnyye Polozheniya Sinop-
tieheslcogo Metoda Dolgosrochnrkh Prognozov Pogody (Fundamentals of the
Synoptic Method of Long-Range'
ong-Range Weather Forecasting), Moscow, 1933, is
generally considered difficult to read -- apparently because it presents
no statistical data, but rather a procedure for the analysis of data for
the purpose of extracting information on the laws of the circulation of
the atmosphere -- this article describes the book as a valuable work guide
which should be re-evaluated in the light of most recent developments in
meteors` ? .
The article also further develops the two principal hypotheses advanced
by Mul'tanovskiy, namely, the hypothesis regarding the "dominator," i.e.,
that the general transfer of air masses in a moving bans formation is made
up of its closed circulation and the general transport of it by atmospheric
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currents, which can be estimated on the basis of the trajectory of the
cyclone; and the hrpothesis that all baric formations on synoptic charts
reflect the activity of larger formations of. synoptical or (As Mul'tanovskiy
called it) dynamic centers of activity of the atmosphere (not climatic).
It is recommended that the book by Mul'tanovskiy be reissued and used
by synopticists. ("The Principles of the Synoptical Method of B. P. Mul'-
tanovskiy for Preparing Long-Range Weather Forecasts," by N. A. Bul:i-nskaya;
Trudy Morskogo Gidrofizicheskogo Institute, Vol. 12, 1958) pp 3-21)
Study on the Formation of Advective Condensation Mists Over Snow Cover
As part of a program of 1956 observations of the physical processes
in the lower atmosphere, this article describes the conditions under which
the formation of advective condensat;.on mists over snow is possible. Such
mists have been observed inVinber on the shores af. the nrn seas, where snow covers
have been considerably earlier than the freezing of the water, and in the
Central Arctic where such occurrences have been observed during the entire
6 months of cold weather.
To predict a mist according to the nomogram of a day on which advec-
tion is assumed or probable, the following data are required:
1. The temperature of the water during the period of advection; since
the temperature of the water surface changes relatively little from day
to day, it is possible to use the mean daily temperature of the water dur-
ing the 24-hour period preceding the advection.
2. The relative humiclity'of the air mass; if the prognosis of of the
relative humidity is not possible, it should be assumed to be 90 percent.
3. The minimum temperature at the surface of the snow in the period
of advection.
No verification of nomograms on the basis of experimental data was
attempted because of the difficulty of selecting material (infT-equent
occurrence of -mists of this tyre). ("Advective Condensation Mists Over
the Surface of a Snow Cover," by L. A. Klyuchnikova; Leningrad, Trudy
Glavnoy Geofizicheskoy Observatorii, No 77, 1958, pp 3-6)
Devices for Measuring Temperature and Humidity Gradients Developed at Pulkovo
Observatory
To increase the accuracy and?convenieuce of operation of instruments in
use at the Main Geophysical Observatory, two simple, compact devices were
developed, with which it is possible, by remote, means, to measure temperature
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and humidity and to conduct all of the other operations connected with
these measurements. One of these psychrometric devices was designed for
use close above the s?irface of water, and the other was mounted on a
television tower. Laboratory tests and practical tests at Koltushakh
and on Lake Sevan,showed that the accuracy of the temperature measurements
of the remote psychrometers is on a par with that of larger models. ("De-
vtce for Measuring Temperature and Humidity Gradients," by N. V. Kucherov:
Leningrad, Trudy Glavnoy Geofizicheskoy Observatorii,, No 77, 1958, pp 57-64)
Wind Velocity Computations For Nonsteady Pressure Fields
At the present time, according to this author, there is no method of
computing the velocity of the' wind in a boundary layer when the pressure.
field is changing; consequently, even with a series of synoptical surface
charts at hand, the velocity of the wind at the height of a weather vane
or wind sock when the pressure field is not steady, cannot be computed-.
The problem was treated earlier by Dyubyuk (Trudy TsIP, No 15) 1949),
who presented a solution in principle, but not an acceptable practical
method of calculation. This article, represents an attempt to derive
formulas, suitable for practicaluse, which wII1 provide a correction for the
velocity of the wind in the case of a nonsteady pressure-field. ("The
Influence of an Unstable Pressure Field on the Distribution of Wind in a
Boundary Layer," by V. Shnaydman; Leningrad, Trudy Glavnoy ueoiizicheskoy
Observatorii, No'77, 1958, pp 65-71)
V. ARCTIC AND ANTARCTIC
Academy of Sciences USSR Publishes Reports on Antarctic
The Trudy Kompl-,;ksnoy Antarkticheskoy Ekspeditsii Akademii Nauk SSSR
(Reports of the Complex Antarctic Expedition of the Academy of Sciences
USSR) are being published by the Council for Antarctic Research, Academy
of Sciences USSR, in the form of several series. Scientific reports on
various types of antarctic research will be included in the series Scien-
tific Articles on Geophysics, Scientific'Articles on Oceanology., and
others.
The series Research Reports and Materials includes a volume containing
results of meteorological and aerological observations made on the Ob' dur-
ing its fLrst voyage to the Antarrctic. An appendix to this volume also
gives the results of meteorological observations conducted on the Lena and
at the station Mirnyy.
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During the period from 10 December 1955 to 26 April 1956, the aero-
meteorological detachment of the First Antarctic Expedition conducted a
total of 1,219 meteorological observations, 182 radiosonde observations,
and 244 pilot-balloon observai;ions. The book contains detailed tables,
listing the coordinates for each point at which observations were conducted
and the hydrometeorological data ':hus obtained.
Another volume in the series Research. Reports and Materials contains
the results of hydrological, hydrochemical, geological, and biological
studies conducted during the first voyage of the Ob' in 1955-1956. The
book lists the names of all scientific associates who participated in
preparing the material for publication.
The volume entitled Description of Expedition on the Diesel-Electric
Ship Ob' 1955-1956 contains an account of the work of the marine expedition,
describing the aims and problems of the expedition. A special chapter of
this volume describes the conditions under which the Qb' sailed from Kalinin-
grad to the Antarctic, the semrch far a site for setting up the Mirnyy observa-
tory, and the weather conditions during the voyage and the period of anchor-
age in Farr,Bay and near Mirnyy.
Other chapters in this volume contain the materials of scientific
observations of the marine expedition. During the period from 30 November
1955 to 8 July 1956, the Ob' traveled 33,325 miles. Scientific observa-
tions were conducted almost continuously.
The volume contains the materials of scientific research on aerology,
meteorology and actinometry, hydrology and hydrochemistry (physical and
chemical characteristics of water masses and currents, color.and trans-
parency of water, wave characteristics, quantity and drift of ice), marine
geology (bottom relief, accumulation of deposits, seismo-acoustic research,
etc.), geophysics (measurements of gravity and electricity in the ocean),
hydrography (geodetic and astronomic observations), and hydrobiology (plank-
ton, benthos, fishes, marine mammals, and birds).
The conclusions drawn from the scientific research work are of a
preliminary nature, as they are based on the first processing of materials
obtained during the period of the voyage. (Trudy Kompl6ksnoy Antarktiche-
skoy Ekspeditsii Akademii Nauk SSSR, Leningrad, 1958)
Activities at Station Vostok
The new group of scientific workers at station Vostok is spending their
fifth month at that location. The middle of the polar night is approaviaing.
The sun has not been seen for over 5 weeks. More and more frequently the
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cLir temperature drops below minus 70 degrees. Heavy snowstorms occur from
time to time. Even when the wind reaches a velocity of only 8-10 meters
pcr second, the air is so saturated with snow dust that visibility is
reduced to a few meters. The atmospheric pressure, which is normally low
at this station (3,420 meters above sea level), is subject to even greater
drops.
As a result of efficient preparations for the polar night, outdoors
work is now reduced to a minimum. Remote-control and automatic instruments
make it possible to work without leaving the building. The time spent
outdoors by the scientists is reduced to 20-30 minutes per day. Only the
launching of radiosondes, meteorological observations, processing of snow
or ice for obtaining water, and some emergency operations require the men
to spend longer periods of time outdoors.
The station is conducting an extensive series of scientific observa-
tions in aerology, meteorology, actinometry, terrestrial magnetism, iono-
sphere, and auroras. The data obtained are transmitted regularly by radio
to the Mirnyy observatory. ("Altitude Above Sea Level 3,420 Meters";
Moscow, Vodnyy Transport, 6 Jun 59)
Results of Third Antarctic Expedition Discussed
The results of scientific work conducted in Antarctica under the
IGY program were discussed on 12 Jun., by the Presidium of the Academy of
Sciences USSR. A report was made by Ye. I. Tolstikov, chief of-the Third
Continental Expedition.
Valuable data have been obtained, which contribute 9, great deal to
the available information on geophysical phenomena and the nature of the
Antarctic. On the basis of seismic and gravimetric measurements, an
interesting theory was suggested concerning the gradual lowering of the
eastern portion of Antarctica under the pressure of the huge mass of ice.
The exploration of the Antarctic ice cap on a cross-section between
the Mirnyy observatory and the pole of relative inaccessibility, covering
over 2,100 kilometers, was of special significance in the work of the
Third Continental Expedition.
The Presidium of the Academy of Sciences USSR approved the work of
Soviet antarctic expeditions., as well as the general direction of future
activities pertaining to the study of the Sixth Continent, as outlined in
the plan for 1959-1965. ("Soviet Scientists Explore Antarctica"; Moscow,
Pravda, 13 Jun 59)
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