INFORMATION ON SOVIET BLOC INTERNATIONAL GEOPHYSICAL COOPERATION - - 1959

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP82-00141R000200570001-0
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 23
• Document Creation Date: November 9, 2016
• Document Release Date: February 1, 1999
• Sequence Number: 1
• Publication Date: March 6, 1959
• Content Type: REPORT

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INFORMATION ON SOVIET BLOC INTERNATIONAL GEOPHYSICAL COOPERATION -- 1959
March 6, 1959
U. S. DEPARTMENT OF COMMERCE
Office of Technical Services
Washington 25, D.C.
Published Weekly
Subscription Price $12.00 for the Series
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PLEASE NOTE
This report presents unevaluated information on Soviet-Bloc
activities in the International Geophysical Cooperation program
from foreign-language publications as indicated in parentheses.
It is published as an aid to United States Government research.
ATIONAL GEOPHYSICAL COOPERATION" PROGRAM --
SOVIET-BLOC ACTIVITIES
Table of Contents
Page
1.
Rockets and Artificial Earth Satellites
1
II.
Upper Atmosphere
13
III.
Meteorology
13
IV.
Gravimetry
17
V.
Arctic and Antarctic
18
a-
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Alpert Discusses Satellite Studies of the Ionosphere
One of the problems which can be directly solved with the aid of arti-
ficial earth satellites is the study of the ionosphere. During its life-
time, a satellite traverses the entire outer part of the ionosphere and then
falls to Earth as a meteorite, or, burning like a meteor, ends its exist-
ence in the lower layers of the ionosphere.
Prof Ya. L. Al'pert, Scientific Research Institute of Terrestrial
Magnetism, the Ionosphere, and Radio Wave Propagation (NIZMIR) had the
following to say on the direction of the investigations of the ionosphere
being followed at preeent.
The ionosphere is the ionized part of the atmosphere, containing, in
addition to neutral particles, free electrons and. ions. Such a medium is
called a plasma. It is characterized by clearly expressed electromagnetic
properties. This is mainly why the ionosphere has such a great effect on
the propagation of radio waves, and it is the use of the latter which is
the most effective way of investigating its properties.
This ionization is found in the atmosphere beginning at a height of
60-80 kilometers. lyre the electron concentration N consists, in various
conditions, of hundreds to thousands of free charges per cubic centimeter.
Gradually changing with altitude, the more of less complex form of N grows
and reaches a maximum value NM at a certain altitude. The value of NM in
the region of this main maximum in the ionosphere changes, for example, in
the middle latitudes under different conditions within the limits of one
up to several millions per cubic centimeter. The greatest value of NM
observed is about 5 x l06 electrons per cubic centimeter. The height of
the main maximum of ionization varies in relation to the time of day and
the latitude and longitude within the limits of 250-400 kilometers.
The electron concentration above the main maximum NM remained unknown
up to the advent of the artificial satellites. The study of the relation-
ship of the electron concentration to altitude is also one of the basic
problems solved with the aid of satellites. Data of this value in the
outer ionosphere was obtained for the first time from observations of
Sputnik I's radio signals.
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Despite the fact that the ionosphere has already been systematically
studied for more than 30 years, there is as yet nn sufficiently complete
and sound theory on its formation and, in many regards, its structure re-
mains obscure. This is related, to the fact that little is known on how
the Sun's radiation interacts with the gases composing the atmosphere and
how the ionization balance in the atmosphere is established.
The composition of this radiation and the nature of the changes in
its intensity at different altitudes is not accurately known. There still
is insufficient information concerning the structure of the atmosphere as
a whole, on the density of neutral particles, on their chemical composi-
tion, temperature, etc., and, in particular, concerning the high regions
of the ionosphere.
Another parameter of the ionosphere, a knowledge of which is very
important is v, the effective frequency of the collisions of electrons
with other heavier particles of gas. The value v depends on how fre-
quently the collisions with ions or neutral particles occur, the temper-
ature of the gas, and the density of the neutral particles and ions.
Without a knowledge of the value of v, it is impossible to calculate
such phenomena as the attenuation of radio waves in the ionosphere, the
interaction of different waves between themselves, the action of 'the
waves themselves on the electromagnetic properties of the ionosphere, and
other effects.
At present) very little is known concerning the value v and concern-
ing its changes in the whole depth of the ionosphere, which is connected
with the particular difficulty of finding a method of measuring it directly.
It is only known that the value of v is of an order of 107 at altitudes
of 65-80 kilometers, ',r ,;., (0.4-5) x 105 at altitudes of 100-130 kilometers
and v = (1-3) x 103 in the region c:` the height of the main maximum of the
ionosphere. In not one experiment was there obtained, even for any condi-
tion, a complete relationship of v to altitude. Also not definitely known
is where collisions of electrons with ions instead of with neutral particles
begin to prevail, a fact that is necessary for understanding the character
of the microprocesses in the ionosphere and, in particular, can help' in
determining the relationship of temperature to altitude, which is extremely
difficult to compute for high regions of the atmosphere. This is explained
by the fact that with a rise in temperature the number of collisions of
electrons with neutral particles increases, and the number of collisions
with ions, on the other hand, decreases.
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Still another important group of problems connected with small-scale
heterogeneity of the ionosphere remains. At present, it can be considered
conclusive that in any limited part of the ionosphere, in a column with a
diameter of several hundred meters and more, extending from its base up
to the height of maximum electron concentration, there is always contained
a great number of small-scale heterogeneous formations, the condensations
and rarefactions of electron density. Studies of these heterogeneous for-
mations or ionized clouds by means of radio wave propagation throughout
the whole thickness of the ionosphere reveals that they have certain sta-
tistical regularities. They have a rather wide range of sizes , chang-
ing within the limits of several tens to many hundreds of meters. It has
been established that in the region from the 110-130 kilometer altitude
up to the main maximum values of eo of an order of 200-300 meters are
encountered. The assumption recently arose that in the lowest altitudes,
heterogeneties with linear measurements of only several meters are ob-
served. These heterogeneities play an important role in ultrashort wave
transmissions over great distances.
Heterogeneous ionospheric formations continuously appear ana 'Usappear.
They move with a probable velocity, relative to the observer of vol chang-
ing within the limits of 2-5 meters per second. They are characterized by
fluctuations of the electron concentration N. that is a N, reaching
several percent.
It is still not clear whether the statistical properties of the iono-
sphere are indications of its pecularities or whether they are the results
of the total interaction of all the heterogeneities at different levels in
a column of the ionosphere taking part in the transmission of radio waves;
thus the parameters of heterogeneities must change strongly with altitude.
Two possible mechanisms for the perturbation of small-scale heteroge-
neities in the ionosphere are turbulence of the ionosphere caused by the
drifting of large regions and drawn out plasma waves, the result of the
formation in them at any moment of a macroscopic region of surplus-charge
electrons. In the latter case, the characteristic size of the heteroge=
neities scattering radio waves is the wave length k of these longitudinal
waves. X grows with a rise in the temperature T of the medium and
changes with an increase of the electron concentration N and the velocity
vo. Thus, if T=1.,500 degrees and 300 degrees, and N=2 x 106 and 2 x 105,
the values which are observed at about the altitudes of the main maximum
of electron concentration and the altitude Z at 110-130 kilometers, then
with vo equal to 2-5 meters per second, values of 200-300 meters are ob-
tained for the wave length , which concides with the sizes of the
heterogeneities eo determined in the experiment.
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Values, characterizing a heterogenous ionosphere and its relationship
to altitude are closely tied to the study of its mechanisms, and that is
why it is hoped this interesting problem will be solved by artificial earth
satellites traveling in particular, almost horizontal, sectors of their
orbits. High-altitude rockets are obviously less suitable for such experi-
ments.
Experimental data obtained, characterizing the various processes in
the plasma-ionosphere, on their part should contribute to the creation of
a general physical theory of plasma waves and turbulence. This theory is
still very little developed, particularly because of its great mathematical
complexity and, in a known degree, because of the insufficient quantity of
experimental data which could have been used as a base for their develop-
ment.
A number of circumstances should be mentioned which it is necessary
to consider in evaluating the application of the various methods and their
accuracy and also for explaining the nature of the investigated values.
First, in radio wave investigations, direct measurement of this or any
parameter of the medium at a given point is not considered. R^.ther, the
values obtained are determined as an average of the values for a certain
region in the neighborhood of a given point. The linear measurements of
this region consist, as a rule, of the many wave lengths of the radio
oscillations being used and in each separate case can be evaluated. Thus
the radius of this region at a distance of about 300 kilometers from the
radiator and a wave length of about 7 meters is approximately 1.5 kilo-
meters.
Second, measurements are hampered by the complexity of the effects
which arise in the neighborhood of the satellite and the nature of its
interaction with the plasma. The phenomena arising in this manner have
as yet been little analyzed theoretically. The thermal velocities of
neutral particles of the atmosphere and ions at great altitudes are 1-1.5
kilometers per second, that is somewhat less then the velocity of the
satellite, which is equal to about 8 kilometers per second. This means
that in a certain cone-shaped area at the rear of the satellite a thinning
of these particles occurs as the satellite passes them. On the other hand,
the velocities of electrons here are 100-150 kilometers per second, that
is, by far exceeding the velocities of the neutral particles. The thinned
region can be filled by electrons flowing into this vacuum and cause an
excess of electron concentration here, that is, a certain negative spatial
charge, which will be diffused into the plasma in a oscillatory manner.
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A negative charge is thus also acquired by the satellite. A "heteroge-
neous cloud," complex in structure, forms in the neighborhood of the satel-
lite. The dimensions of this cloud can be rather large if we consider that
the length of the free run of the particles is very large; thus, at alti-
tudes of 300, 400, and 600 kilometers, they are equal to 6, 20, and 2,000
kilometers, respectively. Therefore, the lifetime of particles at dis-
tances equal to the length of the free run, lasts many seconds. The satel-
lite, during this time, travels hundreds of kilometers so that this cloud
arising in its path forms a trail which lasts for some time and can exert
a marked effect on the results of the measurements.
In the selection of ref;earch methods, the properties of the satellite
itself, and the nature of its interaction with the medium, should be con-
sidered first of all. Peculiarities of this flying laboratory are its
great speed with relatively slow changes in its height while passing over
the point of observation, the disappearance and appearance of both optical
and radio visibility during each passage of the satellite, etc.
Because of the satellite's great speed, the frequency of its radio
signals received by the observer on Earth are somewhat changed. This so-
called doppler shifting of frequencies makes it possible to determine (in
the case of a homogeneous medium) the coefficient of refraction of the
medium and thereby its electron concentration, if the radial velocity of
the satellite's radio transmitter and its frequency are known.
For example, if the ionosphere were homogeneous and its electron con-
centration were 5 x 106 electrons per cubic centimeter, then the doppler
shifting during the satellite's passage would change from zero (when the
satellite is at zenith) to 400-500 oscillations per second (when the satel-
lite is over the horizon).
In a heterogeneous medium, as is the case for the ionosphere (because
of the change N(z) of electron concentration with altitude), it is possible
to determine directly the number of electrons in a column of unit cross
section area extending from the observation point to the radiator. Thus,
in actual conditions, the maximum values doppler frequencies can attain
with a consideration of N(z) are several times less than the above-indicated
values.
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However, direct measurements of doppler frequencies are insufficiently
accurate. This accuracy depends, first of all,. on the uniformity of the
frequencies of two independent sources of oscillations located correspond-
ingly at the point of observation and on the satellite, and cannot be suf-
ficiently high over a long period of time. For increasing the accuracy,
it is necessary to control the source of radiation located in the satel-
lite from the Earth. In this way, the oscillations being compared at the
point of observation will be synchronized or cohered. Values which are of
interest to us can be determined with considerably greater accuracy in this
manner. Use of the coherent doppler method also decreases the error caused
by an incorrect knowledge, at each given moment, of the radial velocity of
one satellite for which it is necessary to register coherent doppler oscil-
lations simultaneously in two frequencies. The results of these experiments
make it possible to study other parameters of the ionosphere. Thus, by
determining, by the indicated method, the number of electrons during the
passage of the satellite in the neighborhood of the zenith, it is possible
according to the change of this value because of the ellipticity of the
satellite's orbit, to determine under quiet ionospheric conditions the
electron concentration at the highest passages of the satellite.
Because of the influence of ionized clouds (the heterogeneities men-
tioned above) a schematic representation of the oscillations being com-
pared on the ground will be in the form of alternately "compressed" and
"expanded" waves, that is, the low-frequency oscillations obtained as a
result of the addition of oscillations radiated by the satellite and the
apparatus on the ground will have a period changing with time. A simple
analysis of such an oscillogram reduced to a determination according to
its median values of minimum and maximum periods and the time interval
between them determines the parameters which characterize the small-scale
heterogeneity of the ionosphere, that is, the values of eo and , N, men-
tioned above.
The doppler effect can be used to conduct wide investigations of
the ionosphere.
A certain peculiarity of the doppler effect can be used for determin-
ing the total electron ccT entration. This peculiarity appears because of
the influence of the Earth's magnetic field on the propagation of radio
waves in the ionosphere. The corresponding effect can be called the rota-
tional doppler effect.
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As a result of the influence of the magnetic field, the ionosphere be-
comes a double-refracting medium leading to the excitation of two waves in
it, instead of one. Each of these waves has its own coefficient of refrac-
tion and, consequently, different doppler shift frequencies. The result
of this is that the amplitude of the satellite signals being received change
with time proportionally to the differences of these frequencies. Under
actual conditions, this difference in frequency can be from zero (when the
satellite is at zenith) to approximately one or less oscillations per sec-
ond. These slow oscillations in the amplitude of the signals being re-
ceived, the frequency of which cs,n be measured with great accuracy, also
make it possible to determine the total number of electrons in a column
of a unit cross iection.
Another method of investigating the electron concentration of the
outer ionosphere, partially used in radio observations of Sputnik 1, is
that of observations of the "radiorise" and "radioset" of a satellite.
During the change in location of a satellite over the point of observa-
tion, the trajectory of its radio waves received on the ground is bent op-
posite the direction the satellite is moving. If the frequency of these
waves is great in comparison to the so called critical frequency of the
ionosphere, which depends on the value of the electron concentration at
the altitude of its main maximum, then the propagation of radio waves is
near that of the optical and the corresponding trajectory represents a
direct line joining the point of observation with the satellite. In this
case, the maximum horizontal distance of the receptioncc' signals from the
satellite is practically equal to the distance opticallyr of its visibility.
If the frequency of the wave is not too great, then the distortion of the
wave's trajectory results in the horizontal distance of the reception of
the radio waves becoming greater than the optical distance. This means
that the "radioset" of a satellite begins later, and the "radiorise," to
the contrary, begins earlier than the visible set and rise.
Assume that the values of the maximum distance (according to the data
of the true orbit of the satellite) and the state of the atmosphere up to
its main maximum, according to the data of an ionospheric station network,
are known for the corresponding moments of the "radiorise" and radioset" of
a satellite flying over the main maximum of electron concentration. Then,
it is possible to calculate how the electron concentration in the outer
? ionosphere must change so that the experimentally obtained values for the
maximum distance for the reception of the radio signals may be observed.
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The relationship of the electron concentration to altitude in the outer
ionosphere can be determined by the indicated method. This makes it pos-
sible to form a presentation on the change in these heights and other values,
for example, the density of neutral particles, which it is. possible to
evaluate as a result of calculating the lifetime of the free electrons and
the time between the different acts of ionization.
As the lifetime of electrons in the outer ionosphere is more than 24
hours, that is, it considerably exceeds the duration of a day and a night,
it is obvious that the state of gases in this part of the atmosphere de-
pends very little on the position of the Earth relative to the Sun, and is
almost quasi-stationary. It is possible to show that under these condi-
tions, the density of neutral particles is proportional to the ratio of
the above-indicated time, as a result of which it is possible to estimate
it according to the value of the electron concentration. ("The Ionosphere
and Artificial Earth Satellites," by Prof Ya. L. Al'pert, Scientific Re-
search Institute of Terrestrial Magnetism, the Ionosphere and Radio Wave
Propagation; Moscow, Priroda, No 10, Oct 58, pp 71-77)
Aeromedicine Discussed in Czechoslovakia
The following is a complete translation of the article "Biological
Problems of Interplanetary Flight and Our Research," by Dr Josef Dvorak
of the Institute of Aero Medicine, Prague.
The launching of the Soviet cosmic rocket -- the first artificial
planet -- clearly indicated the importance of the problem of preparing
for manned flight, at first in artificial satellites and later even further,
into interstellar space. A considerable part of the national income of the
major powers is devoted to research on rocket technology. Certainly, none
really believes that any small country could achieve any of its own results
from biological experiments in extraterrestial space. This, however, does
not mean that research in interplanetary flight is the exclusive domain of
the major nations and that it is impossible for us [in Czechoslovakia] to
gain valuable and important results.
Results of research from artificial satellites and meteorological
rockets show that if the technical problems for safeguarding existence in
a hermetically sealed cabin are solved, the effects of the flight itself
are not connected with any changes in the condition of the organism. The
technical solution, however, is an extremely complex problem in actual
practice, particularly for flights in excess of several ` hours. -Conse-
quently, much work remains to be done in laboratories on earth, based on
the results of flights into space.
UPYKGHT
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Which are the most important factors affecting an organism during
extra-terrestrial flight?
1. During blast-off, considerable effects are caused by the force of
gravity, noise, and vibration.
2. During the flight, it is necessary to assure certain hygienic con-
ditions within the cabin -- sufficient pressure, renewal and replacement
of consumed oxygen, removal of waste matter (particularly carbon dioxide
and water), maintenance of certain temperature differentials, and provision
for adequate quantities of water and food. In addition, it is necessary
to work out a definite plan of activity, since the normal 24-hour day cycle
is distorted during flight.
3. In space, the organism is affected by weightlessness and various
form of radiation.
4. In cases of accidents, it is necessary to assure an emergency sup-
ply of oxygen and provide for sufficient time to adopt emergency safety
measures.
5. During re-entry, it is necessary to protect the organism against
deceleration in the atmosphere, and against overheating.
An analysis of the above factors and the establishment of norms and
standards for technical equipment are the province of space medicine, which
is a part of the branch of aeromedicine. Some of the problems are identical
with the problems involved in safeguarding high-altitude .flight in ex-
tremely fast aircraft; others are connected with basic questions in biology
and physiology.
In all of these areas, research work is being carried on in Czechoslo?-
vakia to a greater or lesser degree (for the most part) to a lesser degree).
It would not be correct, however, to underestimate our potentials.
The successes of Czechoslovak geophysicists and astronomers during the IGY
offer convincing proof. Even in other branches, of science, it is possible
and correct -- to a degree corresponding to our potential -- to work on
cosmic problems.
In many branches of the Czechoslovak Academy of Sciences, in school,
medical, and other laboratories, research on a number of biological and
physiological problems is being conducted and has a direct bearing on
space flight. However, the fact that the majority of the work done was
not aimed at interstellar flight and the fact that sometimes various
authors were not even aware of the significance of their work in the field
of cosmic flight testifies to the inadequacy of the centralized organiza-
tion of this type of research.
CPYRGHT
-9-
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Many years ago, noise problems (at the laboratories of the Czechoslovak
Academy of Sciences), the effect of vibration on' the nervous system
(hygienic faculty), and the effects of excessive gravity were thoroughly
investigated. Also, a prototype of a Czechoslovak protective su't against
the effects of excessive gravity (anti-G suit) was developed. In numerous
physiological laboratories, research was conducted on the effects of oxygen
shortage (hypoxia) and the possibility of influencing resistance to hypoxia
in the course of an individual's development. We have in our country a high
altitude suit and a superpressure compensation suit for use in the event
of a crash. Experiments were also carried out In which "boiling" of the
body fluids was investigated in live animals at considerable heights (where
the boiling point drops below 30 degrees Centigrade).
Noteworthy significance has been attained by the work of the biological
laboratories of Academician Malek, which are concerned with the structure
of certain marine plants and their modification. It is presupposed that in
future years, it will be necessary to obtain food from rapid-growing micro-
organisms -- simultaneously it would be possible, through their help, to
renew the air in the cabins of rockets. A solution to this question could
fundamentally change the method of renewing the air in interplanetary
rockets. A great deal of work, especially in the physiology laboratories,
has been devoted to questions on the effect of a change in the work period,
lack of sleep, fatigue, heat, and protection against it. A special suit
was also tested for use under conditions of extreme heat. The possibilities
of the application of these results are obvious.
The dynamic weightless state was achieved in our country for the first
time early in the 1950s during rests with aircraft. The significance of
this was not comprehended by anyone at the time. The influence of rapid
alternation between excess gravity and weightlessness lasting several sec-
onds was also investigated. The results attained are in agreement with
those of today. It was learned that weightlessness does not affect the
proper muscle coordination in small movements. Furthermore, it was found
that 10 percent of the experime:ital personnel got "air sick". as a result
of the irritation of the sense of equilibrium in the middle ear. It was
clearly confirmed that it is necessary to select pilots for flights.
The effect of radiation has been the object of basic research in our
country for some decades, and it is associated primarily with the name of
a Corresponding Member of the Czechoslovak Academy of Sciences, Hercik.
CPYRGHT
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 CPYRGHT
CPYRGH1
At a recent congress of flight physicians in Lovan, which concerned
problems in cosmic medicine, it was shown that the main share of research
the above-mentioned problems will be borne by work in artificial satel-
lites. From this viewpoint, our results are modest but not, however, in-
significant. Even with today's means, it would be possible to substantial)
increase the usefulness of the results obtained for interplanetary flights,
if the work was well coordinated.
It would be immodest and unrealistic to count on independent work dur-
ing actual interplanetary flight in the near future in our country. There
is, however, a series of problems the solution for which we have very good
prerequisites. They are, for instance, problems of cultivating plant micro-
organisms under conditions of motion, influencing their material changes
and composition, mastering their growth; problems of enzymatic processes
during the dissolution of carbon dioxide; the production of food, such as
carbohydrates, fats, and proteins, directly from inorganic components, with
the exclusion of plants; problems of protection from noise and heat; prob-
lems of ensuring microclimate in confined areas; the influence of various
types of radiation; the influence on the normal processes in an organism
during the course of the day; the processes of acclimation to new living
conditions, etc.
Interplanetary flights will provide the development of science with
an unusually significant stimulus. It would be proper to incorporate this
kind of work in a unified plan and thus help to attain results which would
correspond to the position of our science in the world.
A photograph accompanying the articl is ca tioned Czechoslovak
ona ro t - ("Biological Problems of Inter-
planetary Flight and Our Research," by Dr Josef Dvorak, Institute of Aero-
medicine; Prague, Rude Pravo, 18 Jan 1959, p 4+)
New Soviet Satellite? Signals Picket Up in Belgium
Jadoule, an arwteur radio operator from Boitsfort, has stated that he
twice heard signals broadcast by a satellite on the frequency of 20.005
kilocycles on 5 February. It was certainly a satellite broadcast, he says,
because the Doppler effect was very distinct. He heard these signals from
1951 to 1959 hours. The signals were broadcast on a nonmodulated frequency:
onedash ("traLt")1bUowed7y threecr four (groups?] made up of five short bars
("barre"), or one dash ("traittiti) followed by another bar ("barre"), repeated
several times. Jadoule recorded the signals received at 2131 hours. ("A
New Russian Satellite? Radio Signals Picked Up in Belgium"; Brussels, La
Libre Belgique, 7/8 Feb 59, p 3)
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Model of "Mechta" To Be Displayed At Leipzig--Spring Fair
A model of the USSR's first Moon rocket, "Mechta," which became the
first artificial planet, will be displayed publicly for the first time at
the Leipzig Spi'ing Fair, 1-10 March. Models of Sputniks, 1, II and III:
will also be exhibited there. (Helsinki, Hufvudstadabladet, 12 Feb 59,
p 5)
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Radiotelescope With Scanning Radiation Pattern At Crimean Observatory
A radiotelescope for continuous observation of the Sun's radio
emission has been installed at the Crimean Astrophysical observa-
tory. Such observations were conducted on the 10-centimeter wave. The
telescope was mounted on a parallactic stand, which facilitated automa-
tic tracking of the Sun. The required noise immunity was attained by
modulating the signal with an oscillating radiation pattern. The an-
tenna assembly of the telescope consists of a truncated parabolic re-
flector with two horn radiators. The radiators are connected by a
section of rectangular wave guide in such a manner that the planes of
polarization are mutually perpendicular. A ferrite stub with a porce-
lain activator is mounted in the wave guide. Under the action of a
variable magnetic field the ferrite stub rotates the p7^ne of polariza-
tion in the wave guide by ? 45 degrees.
The radiotelescope is calibrated with the aid of a noise generator,
which is mounted in the place of one of the radiators. The modulation
frequency is 180 cycles. Sensitivity of the radiotelescope for the fre-
quency band of 2.5 megacycles and a time constant of 3 seconds is 4-5
degrees. The effective antenna area is 13 square meters. The Sun's
radio emission is recorded on a paper tape.
The design of the individual mechanical components of the radio-
telescope was done by B. P. Abrazhevskiy and the radioengineering com-
ponents by V. A. Yefanov, and P. N. Stezhka. ("Radiotelescope With
Scanning Radiation Pattern Operating on 10 cm Wave," by I. G. Moiseyev,
Gor'kiy, Crimean Astrophysical Observatory, Academy of Sciences USSR,
Izvestiya Vysshikh Uchebnykh Zavedeniy, Radiofizika, No 3) 1958, pp
159-161)
III. METEOROLOGY
Subcoamnission,on Actinometry and Atmospheric Optics Organized Under
Academy of Sciences USSR
A Subcommission on Actinometry and Atmospheric Optics (Podkomissiya
po Aktinometrii i Atmosfernoy Optike) has been organized within the Com-
mission on the Physics of the Atmosphere under the Department of Physi-
coma,thematical Sciences, Academy of Sciences USSR. The following sci-
entists are members of the subcommission: K. Ya. Kondrat'yev, chairman
(Leningrad State University); G. V. Rozenberg, deputy chairman (Institute
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of the Physics of the Atniospherc, Academy of Sciences USSR); K. S. Shifrin
(Main Geophysical Observatory); Yu. D. Yanishevskiy (Main Geophysical Ob-
servatory); G. K. Sulakvelidze (Institute of Applied Geophysics) Academy
of Sciences USSR); and V. G. Kastrov (Central Aerological Observatory).
The subcormnission's task is to collect information on works concern-
ing the study of radiation conducted at various points and establishments,
and to prepare suggestions for the development and coordination of these
works. The subcommission will also prepare reports and observations on
the study of radiation, etc., which has been condudted in the USSR.
The subcommission has intentions of convoking a conference on act-
inometry and atmospheric optics either late in 1958 or in early 1959.
("In the Commission on the Physics of the Atmosphere Under the Academy
of Sciences USSR)" Leningrad, Meteorologiya i Gidrologiya, No 11, Nov 58,
p 69)
Conference of Subcommission on Actinometry and Atmospheric Optics, Academy
of Sciences
A scientific conference held in Leningrad during the week ending
6 February was devoted to the most important problems of the study of
radiant energy in the atmosphere (actinometry) and atmospheric optics.
The conference was called by the Commission on the Physics of the At-
mosphere of the Academy of Sciences USSR, the Main Geophysical Observa-
tory, and Leningrad University. Representatives of the scientific re-
search institutions of many cities in the USSR, and also scientists from
China, Poland, the German Democratic Republic, Czechoslovakia' and the
Korean People's Democratic Republic, participated in the work of the con-
ference.
The ever-growing importance of actinometric investigations for
meteorology, agriculture, helioengineering, medicine, and other fields
of the national economy and science was emphasized in reports by A. M.
Obukhov, Corresponding Member of the Academy of Sciences USSR; K. Ya.
Kondrat'yev, prorector of Leningrad University; Yu. D. Yanishevskiy,
senior scientific associate of the Main Geophysical Observatory; and
others.
Problems on the distribution of the Sun's radiant energy on the
earth, the study of the transparency of the atmosphere, the possibility
of measuring sunlight, moonlight, and other exoatmospheric light were
discussed by the participants. A special session dealt with the effect
of radiant energy on the longevity of building construction and the
calculation of radiation in designing housing. ("Study of Radiant
Energy": Moscow, Izvestiya, 7 Feb 59, p 4)
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Soviet IGY Expedition Studies 'Atmospheric Conditions in Egyptian Desert
A study of atmospheric conditions in the Libysn: Desert south of
Aswan was made in connection with the IGY program by a Soviet group dur-
ing October and November 1957. The station was set up one kilometer from
the Nile and 200 kilometers from the Red Sea. The exceptional stability
of the atmosphere for several hours before and after midday was noted.
Measurements of polarization were made as a sensitive index on this sta-
bility. ("Scattering and Polarization, of light by the Atmosphere in the
Libyan Desert," by Ye. V. Pyaskovskaya-Fesenkova; Moscow, Poklady Akademii
Nauk SSSR, Vol 123, No 2, 11 Nov 58, pp 269-271 " '
Changes in the Color of the Twilight Sky
Photoelectric measurements of the distribution of the energy of a
twilight sky at zenith were made with the aim of explaining the reasons
for changes in the color of the sky. The results were compared with
theoretical calculations.
A comparison of the'calculated values of brightness with the observed
values shows that the intensity of the observed twilight luminescence in
all wave lengths in the visible part of the spectrum is rather close to
the intensity of first order scattered radiation only in the intervals of
setting of the Sun from 0 to 6.5 degrees. Beginning with 8.5 degrees, fLrst
order scattering plays a negligible role in the total flow of radiation in
the sky at zenith in all parts of the visible spectrum. Color temperatures
were used for characteristics of the color of the twilight sky. Because
one value of temperature-cannot represent the distribution of energy in
the part of the spectrum being observed, the spectrum was divided into two
parts: the first, from 370 to 440 microns; - and the second, from 440 to 600
microns.. Color temperature was determined by comparing the observed energy
distribution with the Planck distribution, calculated for a series of tem-
peratures.
The color temperature for the region of the spectrum from 440 to 600
microns changes in relation to the settings of the Sun under the hor~,zon
reaching a maximum value at about 10 degrees. In the blue part of the
spectrum (370-440 microns), these changes-were almost absent. Thus,
changes in the color of the twilight sky in the investigated part of tLz
spectrum are caused mainly by the region from 440 to 600 microns.
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The character of the distribution of energy in the spectrum of the
twilight sky is caused not only by the presence of ozone, but also by
the general character of the absorption of light in the Earth's at-
mosphere. Of particular value in the formation of this spectrum are
the altitudes of th3 so-called twilight rays for different wave lengths.
The relationship of the altitude of an effective twilight ray to the
degrees of setting of the Sun is shown. In the lower degrees of settLag,
the difference in the altitudes of an effective twilight ray for 370
and 700 micron: reaches 20 kilometers. Since the effective twilight
ray for short wave lengths appears above the rays for longer wave radia-
tion at one and the same time, the spectral distribution must be charact-
erized by low intensity in the extreme blue part of the spectrum, in com-
parison with the distribution which corresponds to Rayleigh scattering.
Since the difference in the altitudes of the effective twilight rays
decreased with a progression of the degrees of setting of the Sun, the
relative intensity of the blue radiation increases, and, as a consequence,
the ratios of the intensity in the blue and yellow-green rays must in-
crease.
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In the analysis of the optical properties of the Earth's atmosphere
by the twilight method, it must be considered that rays with different
wave lengths give information on different levels of the atmosphere at
one and the same time. In addition, it is necessary to remember that the
width of a twilight ray is different for different wave lengths. In this
respect, the blue rays are preferable, as their twilight ray is consid-
erably narrower than for the red. Qbhanges in the Color of the Twilight
Sky," by V. B. Divari, Astrophysics Institute, Academy of Sciences Kazakh
SSR; Moscow, Doklady Akademii Naik SSSR, Vol 122, No 5, 1958, pp 795-798)
Theory of Scintillation of Terrestial Light Source Checked Experimentally
The scintillation and flickering of stars and other radiation sources
both within and outside of the earth's atmosphere have recently received
considerable attention in problems connected with astronomical observation
and radiometeorology, the authors note, and a rather complete theory of
these phenomena has been developed.
The results of the theory are summarized as follows for the case when
fluctuations in the index of refraction of the medium are subject to the
"2/3 law."
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1. Fluctuations in light intensity have a logarithm': normal dis-
tribuution.
2. The dispersion of the intensity I of a light wave is given by
the formula
o-, 2 [ln I - In I]2 ^ 10.5 Cn 71-7/6 L11/6,
or o- 2- L11/6, where L is the distance the light travels in the tur-
bulent medium, A is the wave length, and Cn is a constant from the ex-
pression for the fluctuations in the index of refraction n of the medium.
3. The correlation function of the fluctuations of the logarithm
of the light intensity in a plane perpendicular to the ray is a function
of Q/,it-A L , where f is the distance between points of observation.
The correlation is of the order ~L.
4. The frequency spectrum of the fluctuations is a function of
the quantity f 'V ; L/vr,, where f is the frequency and vn is the compon-
ent of the mean wind velocity perpendicular to the ray.
Work carried out during 1956 and 1957 to verify these relationships
experimentally is described. The experiments were made in a level region
aad a light source 2 meters above the earth was used. The values used
for L between the source and the receiver were 250, 500, 1,000, and 2,000
meters. Graphs and tables of the experimental results are given. Agree-
ment with the theoretical predictions was found to be satisfactory.
("Experimental Investigation of the Statistical Characteristics of the
Scintillation of a Terrestial Light Source," by A. S. Gnrvich, V. I. Te,-
tarskiy, and L. R. Tsvang, Institute of Physics of the Atmosphere, Acad-
emy of Sciences USSR; Moscow, Doklady Alcademii Nauk SSSR) Vol 123, No 4,
1 Dec 58, pp 655-658)
Apparatus for Airborne Gravity Surveys Discussed
Recent years have seen great successes in the development and ap-
plication of aerogeophysical methods of prospecting. This has led to
attempts to widen the scope of these methods of prospecting and, in
particular, to develop aerogravimetric meth;;ds. The first steps in
this direction were reportedly made in the US by the invention of the
aerogradientometer and its testing in Canada. Thus, gravimetry has
entered into a new phase of its development, characterized by the
gathering and application of aerogravimetric measurements. Certain con-
siderations on the solution of the problem are presented.
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The various problems faced in the use of airborne gravimeters are
discussed. The use of the second derivative method of gravity interpre-
tation is presented as the most effective means for the development of
aerogravimetric surveying. Two systems of vertical gravitational grad-
ientometers, one based on the use of two weights and the other on the
use of the systems of two identical spring gravimeters are considered
satisfactory for transducer constructions in the condition of flight.
The sy3tem of a double-differential astatic gravimeter appears the
most suitable for the development of an instrument in motion, as changes
due to temperature and the stretching of the springs will occur slowly,
giving a total zero drift to the instrument. In addition, the vertical
acceleration of the supports is completely excluded and the deviation of
the instrument under the action of horizontal accelerations, within rather
considerable limits, will have no effect on the readings of the instrument.
Elementary theoretical consideration confirms the possibility of de-
veloping apparatus for gravimetric surveys while in motion. ("Develop-
ment of Apparatus for Gravimetric Surveys in Motion," by V. V. Fedynskiy)
Institute of the Physics of the Earth, Academy of Sciences USSR; Moscow,
Izvestiya Akademii Nauk SSSR, Seriya Geofizicheskaya, No 1, Jan 59, pp
146-152)
New Mountains Discovered in Antarctic Interior
On returning from a flight into the interior of Antarctica, a
Soviet plane.piloted by Perov passed over a hitherto unexplored region.
Several new discoveries were made during this flight. Quite unexpectedly
a pyramid-shaped, partly snow-covered mountain peak was discovered, 3,300
meters above sea level. Following this, a mountain range consisting of
17 peaks waa discovered. At a point 74-10 1 and 63-20 E. the Soviet ex-
plorers entered a massive, twin-peak mountain on the may.
In addition, six more mountain peaks were discovi;red, which repre-
sent the southern extremity of the Prince Charles mountain range; also
six nunataksr several previously uniaiow.i ice cupolas, and a glacier.
These were important discoveries, since mountains were found in a lo-
cation where a level, uninterrupted ice sheet was believed to exist.
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The overland detachment, moving toward the pole of relative inacces-
sibility, made seismic soundings of the ice thickness. As a result, it
appeared that the elevation of the basic rocks increased toward the center
of East Antarctica. The discovery of previously unknown mountains not only
confirms the accuracy of Soviet seismic soundings, but it also proves that
the basic rocks of East Antarctica are found at a higher elevation than
had been assumed before. This fact supports the theory that Antarctica is
a continent. ("Discoveries of Soviet Explorers"; Leningradskaye. Pravda,
13 Dec 58)
Antarctic Flights and Discoveries
The current Antarctic summer has been unusually severe. There have
been frequent blizzards and purgas. Under these conditions, synoptic
weather forecasts are very important.
On a recent flight into the interior of the continent, a Soviet
plane passed over the central regions of Antarctica, where no human beings
had ever been before. At a point 75 S and 60 E, a hitherto unknown,
pyramid-shaped mountain peak was visible from the air, rising about 3,500
meters above sea level. When the plane turned around in the direction of
Mirnyy, a mountain range was visible on the left side. In a latitudinal
direction, the mountains extended eastward. Over 20 peaks and individual
mountain massifs were discovered in this region. Nothing had been known
before regarding the existence of these mountains.
As soon as the plane returned to Mirnyy, a heavy storm and snowfall
began. A cyclone covering a huge area was approaching the antarctic
coast from the Indian Ocean. Such deep cyclones are very infrequent in
this area, especially during the Antarctic summer. Similar cyclones had
not been recorded by the members of eexlier Soviet expeditions. The wind
velocity at Mirnyy and on Drygalski Island, where weather observations
were being conducted, reached 1E0-50 meters per second. ("A Harsh Summer";
Moscow, Vodnyy Transport, 22 Jan 59)
Current Activities in Antarctica
Soviet scientists will continue their research activities in An-
tarctica during 1959. The transcontinental sled-tractor train which is
to reach three poles -- south geomagnetic, south geographic, and pole
of relative inaccessibility -.. will start in 1959?
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Part of the Fourth Antarctic Expedition has already begun its
activities. Our group arrived in Mirnyy just before New Year's on
the Ob'. The remaining expedition members arrived on 21 January on the
ship Mikhail Kalinin. The latter group included a group of Polish sci-
entists headed by Wojciech Krzeminski. Soviet pilots transported the RiL-
ish scientists by plane and helicopter to the station Oazis, transferred
to the Polish People's Republic by the USSR government.
In the near future, the Mikhail Kalinin will take on board the mem-
bers of the Third Antarctic Expedition who are returning to the USSR.
The staffs at the interior Soviet stations were recently replaced.
The new staff at the station Vostok, which is to spend a year at the
south geomagnetic pole, consists of workers of the Arctic and Antarctic
Institute. V. Ignatov, geophysicist and Candidate of Technical Sciences,
is chief of the station. He and Ya. Baranov, radioman, previously win-
tered at the drift station Severnyy Polyus-7 in the Arctic. A Semochkin,
mechanic, took part in the operation of two drift stations in the Central
Arctic; and D. Nizyayev, magnetologist, participated in a number of high-
latitude expeditions of the Main Administration of the Northern Sea Route.
The new staff which has taken over the station Vostok is continuing to
operate under the IGY program. ("Preparations for Spring"; Moscow, Vodnyy
Transport, 24 Jan 59)
On 10 February, a Polar Aviation airplane piloted by S. A. Petrov
took off from Leningrad for the Arctic. On board the plane was a group
of scientific associates of the Arctic and Antarctic Scientific Research
Institute, headed by A. L. Sokolov, Candidate of Geographic Sciences. The
scientists will study the ice cover of the arctic seas.
During a period of 3 weeks, the "ice reconnaissance team" will have
to fly over 30,000 kilometers under difficult weather conditions. ("Recon-
naissance of Polar Ice"; Moscow, Sovetskaya Aviatsiya) 11 Feb 59)
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