SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INFORMATION

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP82-00141R000200400001-8
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 22
• Document Creation Date: November 9, 2016
• Document Release Date: January 27, 1999
• Sequence Number: 1
• Publication Date: November 7, 1958
• Content Type: REPORT

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PB 131632-39
SOVIET BLOC IIITEM- TIOflAL GEOPHYSICAL YEAR INFORMATION
November 7, 1958
U. S. DEPARTMENT OF COMMERCE
Office of Technical Services
Washington 25, D. C.
Published Ueek1y from February 114, 1958, to January 2, 1959
Subscription Price $10.00 for the Series
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PLEASE NOTE
This report presents unevaluated information on Soviet Bloc
International Geophysical Year activities selected from foreign-
language publicatior.s as indicated in parentheses. It is pub-
lished as an aid to United States Government research.
SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INFORMATION
Table of Contents
Page
I.
Upper Atmosphere
1
II.
Meteorology
9
III.
Seismology
13
IT
Oceanology
14
V.
Arctic and Antarctic
15
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I. UPPER ATMOSPHERE
Soviet Study on Attenuation of Light in the Earth's Atmosphere
A detailed work on the attenuation of light by the earth's atmos-
phere reports on measurements of--the spectral transparency of the at-
mosphere and of the water vapor content in a vertical column through
the entire depth of the atmosphere. The experiments were carried out
with simple observatory instruments. In the observations, which were
conducted in 1954, a single-prism spectrograph with comparatively low
resolution was used. The output slot of the spectrograph (used as a
monochromator) separated about 210 angstroms in the region of one micron.
The energy pickup was a silver sulfide photocell with a very simple bar-
rier layer.
Observations of the spectral transparency :.f the atmosphere on 36
days revealed a dependence of the coefficient of transparency on wave
length in the spectral region of 420-1,010 millimicrons.
On the basis of more than 500 determinations of the water vapor con-
tent throughout the entire depth of the atmosphere, and a measurement of
the absolute humidity at the surface of the earth, the seasonal pattern
of the water vapor content over the entire thickness of the atmosphere
was established and compared with the course of the absolute humidity
at the earth's surface.
The coefficient of correlation between the water vapor content in
a vertical column of the atmosphere and the absolute humidity at the sur-
face was computed as r = 0.87 f 0.03. The equation of regression, ex-
pressing w in terms of q, has the form: w =. 1.92 q + 0.09.
The mean square error of the regression formula is equal.to 0.26 cm
of precipitated water. This indicates that a measurement of the absolute
humidity at the surface of the earth may be used to determine the water
vapor content over the entire thickness of the atmosphere, with an aver-
age error of 0.26 cm of precipitated water.
It is also shown that it is possible., within rather wide limits, to
make use of the root-mean-square law to determine the water vapor content
in relative units according to observed absorption bands in the near in-
frared.
On the basis of observations of the spectral transparency of the
atmosphere, simultaneous determinations of the water vapor content, and
a determination of optical properties, it was possible to separate the
total attenuation of light by the earth's atmosphere into individual
components (molecular scattering, attenuation by water vapor, aerosol.
scattering, etc.).
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In separating the attenuation by water vapor, the Foule coefficients
(; ricattt ring by water vapor at various wave lengths were confirmed.
In connection with observations of the spectral transparency, the
Loschmidt number N was determined -- assuming an anisotropic molecule --
f or days following precipitation, when the attenuation of light by the
earth's atmosphere was caused, in general, only by molecular scattering
and a decrease of water, vapor, which were capable of being distinguished
independently. The Loschmidt number determined, N a (2.68 plus-minus
0.02) .1019 was in agreement with accurate laboratory data (2.686 .1019 ),
which indicates the advantage of the correction for the anisotropic mole-
cule in the calculation of molecular scattering.
It was found that the aerpppl attenuation of light, which was ob-
tained by subtracting the attenuation by water vapor from the total. at-
tenuation of molecular scattering, has three degrees of dependence on
wave length: it can be neutral; it can, increase uniformly with;dLmininsh-
ing wave length; or it can follow an extreme course with a maximum, the
location of which varies for various days and lies within the limits 460-
520 millimicrons.
The author thanks the director of the Department of Atmospheric
Physics of the Astrophysics Institute, Ye. V. Pyaskovskaya-Fesenkova,
for supervising the work, and the senior laboratory associate of the
institute, N. I. Ovchinnikova, who made the observations with the aureole
photometer, ("On the Question of the Role of Various Factors in the At-
tenuation of the Light of the Earth's Atmosphere," by T. P Toropova;
Alma Ata, Izvestiya Astrofizicheskogo Institute Akademiya Nauk Kazakhskoy
SSRI Vol 6, 1958 pp 3-72)
Sino-Soviet Expedition Observes Annular Eclipse of, the Sun
CPYRGHT
"A point expedition, in which 22 Soviet and 31 Chinese specialists
took part, was organized by scientific institutions of the Academy of
Sciences USSR and the Academia Sinica of the Chinese People's Republic
of China.
"Supervision of the expedition was conducted by A. P. Molchanov,
acting for the Academy of Sciences USSR, and Ch'eng Fang-yun, acting
for the Academia Sinica. A special committee, headed by Wu Yu-hsun
vice president of the Academia Sinica, was created for guaranteeing the
work of the expedition. The organization of the expedition in the USSR
came under the supervision of A. A. Mikhaylov, chairman of the Astronomi-
cal Council."
The experiences of the expedition are reported in two parts --- radio
,,.ctronomical observations and optical observation,%- A full translation of
these reports follows
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Radio Astronomical Observations (A. P. Molchanov and Ch'eng Fang-yun)
Radio astronomical observations of solar eclipses, both the full
eclipse and the annular eclipse, are of great interest because of their
ability to isolate radiation from small sources, which at present cannot
be accomplished by other means. In addition, the most important reasons
are the determination of the spectrum and structure of local sources of
both nonpolarized and polarized radiation, the variation of the residual
flow of radio emission during the time of minimum distance between the
centers of the Moon and the Sun, and the investigation of the shape of
the Sun.
The observations of the eclipse in 1958, which was a year of
maximum solar activity, were especially interesting.
The expedition set up seven radiotelescopes, and ,bservations
were conducted over a wide wave range according to a program worked out
under the direction of S. E. Khaykin, chairman of the Commission on
Radio Astronomy of the Astronomical Council, Academy of Sciences USSR.
Groups of associates of the Main Astronomical Observatory (super-
visors A. P. Molchanov and D. V. Korol'kov; radiotelescopes with ranges
of 2,2 cm, ), z 3.2 cm, ), = 3.3 cm, A= 4.5 cm, and ?ti5.1 cm), the Institute
of Physics imeni P. N. Lebedev (supervisor, A. Ye. Salomonovich; radio-
telescope with a range of X_0.3cm), and the Byurakan Observatory of the
Academy of Sciences Armenian SSR (supervisor, E. G. Mirzabekyan; radio-
telescope with a range of A=50 cm), took part in the expedition.
It should be mentioned that almost all of the apparatus were
original designs, and many of the (A.AO.8-2.0-5.1 cm) measured simulta-
neously both the polarized as well as the nonpolarized components, one
(.*3.3 cm) measured the circular and linear polarization, and one (%
3.2 cm) with a scanning device was calculated for the use of new methods
of investigating. radio emissions of the Sun. The apparatus working on
a wave length of a, r50 cm was an interferometer. On a wave length of ;
4.5 cm, it measured only the nonpolarized component of the radiation.
The pv:sence of apparatus wwworldrg on waves shorter than 3 cm and in the
optical range required the careful selection of the expedition's operat-
ing location. Thanks to the special attention accorded the expedition by
various organizations of China, in Canton, and on the island of Hainan,
detailed study of meteorological data was made and several points in
the track of the eclipse were examined. The selection rested on the
region of the city of San-ya, Hainan Island, which was distinguished by
r he low number of hazy days in April and comparatively weak winds. Ob-
ervations confirmed the correctness of the selection. During 1 1/2
onths there were only 3 days of rain.
CPYRGHT
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Observations of the eclipse were successfully carried out with
all the apparatus of the expedition. Some preliminary conclusions can
be drawn until a detailed processing of the records can be made.
In a majority of the equipment (;,,,3.2, 4.5, and 5.1 cm) distinct
variations of the derivative at the moment the sunspots were covered and
uncovered by the lunar disk were registered, which made it possible to
estimate the brightness temperature of local sources of radio emissions
in these regions.
The covering and uncovering of spots produced no variations in
the recording for waves ofao0.8 cm and,Z =2 cm, which would make: it possi-
ble to estimate the upper limits of radio emissions of these sources in
these regions.
Thus, at the same time and under the same conditions, data on a
local source occurring near No :L88 group of spots (numbered according to
the bulletin Solnechn rye Dannyye) on five waves in the centimeter range
(of these, two according to the upper limit) and on a 50 cm wave of the
decimeter range were obtained. These results, apparently for the first
time, give a : r.Liable spectrum cf local sources both in nonpolarized emission
and in circular polarized emission which is of great scientific value,
since only data obtained on several waves simultaneously make it possible
to attempt the calculation of the effective temperature and intensity of
the magnetic field in the lower layers of the Sun's corona.
An analysis of the recordigigs showed that on waves with a3.2, 4+. 5,
5.1 cm the radio emission came from not one single large area over a
group of spots, but from several areas located over the center of spots
and having dimensions of the order of one angular minute. Such a
separation was determined quite distinctly both in nonpolarized emission
as well as in polarized emission according to range (with,'l a.3.3 and 5.1
cm). In the latter case, it was noted that the leader spots corresponded
to the southern pole, and the trailer spots of the groups to the northern
pole, which agreed with the results of the optical observations. However,
the data of radio astronomical observations. are related to considerably
higher layers of the Sun's atmosphere.
The separation of lccal source emission into regions is of great
value for studying coronal condensations in the Sun's atmosphere, to which
at present increased radio emissions are attributed with a high degree of
probability.
The investigation of the radio emission of local sources on a
wave length ofA a3.2 cm was conducted not only according to the variation
of the steepness of the curve of the recording, but also according to the
shifting of the effective center of the Sun's radiation occurring during
the covering and uncovering of the sources (A :3.2 cm). The results of the
observations by these unrelated methods were in good agreement.
CPYRGHT
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Sources in the region of several other spots occurring on the
Sun at the moment of observation were registered in addition to the source
located near the No 188 group of spots.
A well-defined local source of radio emission (registered on a
wave length of ).k.3.2, 4.5, 5.1 cm) occurring at the limb of the disk it-
self and outside of it were of great interest This source could be re-
lated either to the coronal condensation over the No 204 group of spots
located at the time of the observatious on the invisible hemisphere of
the Sun (at a distance of 23? from is limb), or to the area of bright
green lines in the corona in the region of the spots which existed in
the preceeding revolution of the Sun. The circularly polarized radia-
tion component of this source was not registered.
An analysis of curves of the recordings obtained by all of the
apparatus after the introduction of instrument corrections and the elimi-
nation of the influence of local sources makes it possible to estimate
the distribution of "radio brightness" for the solar disk. This problem
is of value for opinions concerning the structure of the upper layers of
the Sun's chromosphere. However it is already possible to make a deduc-
tion concerning the existence of a bright limb on the Sun by the residual
fluxes of radiation for certain waves (,x,.0.8 and 3.2 cm)
The measurement of the "ellipticity" of the Sun on a wave length
of ~ w3.2 cm was made during the observations by a new method with the aid
of conical scanning patterns of the radiotelescope antenna along the limb
of the solar frisk. The obtained recordings registered changes in the'shape
Of the studied part of the Sufn'during the eclipse and for the middle of
the annular phase showed that the ellipticity was insignificant -- less
than the threshold of sensitivity of the apparatus.
Observations on interferometer equipment (A=50 cm) registered
both the polarized emission of the local source near group No 188, as
well as the residual intensity of the emission during the annular phase
which surpassed the uncovered area of the Sun's disk. Much scientific
work was conducted by the associates of the expedition, in addition to
the direct intensive work which is usual for conditions of preparation
for observations of a solar eclipse. The results of the preliminary
processing of the materials of the joint observations were discussed in
a 3-day seminar which was organized in Peiping. Discussions took place
on a number of reports made by the Soviet and Chinese participants in
the observations. The results of the observations were reported in the
ranches of the Academia Sinica in Canton, Shanghai, Nanking and in a
eeting of the prer