SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INFORMATION

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP82-00141R000200270001-3
• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 34
• Document Creation Date: November 9, 2016
• Document Release Date: January 19, 1999
• Sequence Number: 1
• Publication Date: August 8, 1958
• Content Type: REPORT

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SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INFORMATION
August 8, 1958
'U. S. MIPAini it OF CO161EMB
Office of Technical Services
Washington 25, D. C.
Published Weekly from February 14, 1958, to January 2, 1959
Subscription Price $10.00 for the Series
PB 131632-26
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PLEASE NOTE
This report presents unevaluated information on Soviet Bloc
International Geophysical Year activities selected from foreign-
language publications 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
I. Rockets and Artificial Earth Satellites
II. Upper Atmosphere
Page
1
III. Arctic and Antarctic 28
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I. ROCKI';Ta AND ARTIFICIAL EARTH SATE LLITE'S
l?luin Proble: is in Cosmonauti.cs Discussed by Soviet Scientist
Prot' G. V. Petrovich has published an article entitle! "Basic problems
in Coamonautics: in the official organ of the Academy of' Sciences USi SR. The
following is the full text of that article.
Today, when the first stages in the development of rocket problems have
already been passed, when both intracontinental and intercontinental rockets,
as well as artificial Earth satellites, have been built, the queution arises
as to what will the subsequent ctar;eo in the growth of rocket engineering;
be like and what paths will further development of cosmonautico follow?
The achievement of three critical cosmic velocities are fundamental
landmarks in the development of cosmonauticu. The first of these is a
circular velocity (around 8 kilometers per necond), which is the minimum
required for the creation of an artificial Earth satellite; the second
cosmic velocity is parabolic (around 11 kilometers per second), which is the
minitnum required for escaping the Earth and revolvin? as a satellite of
the sun, as an independent planet, and, consequently, also for obtaining;
the possibility of flight to other celestial bodies of our solar system;
the third cosmic velocity is hyperbolic (around 16.'t kilometers per second),
which is the minimum necessary tc escape our solar system forever and to
head for the stars.
By achieving; velocities within the range of approximately 8-11 kilometers
per second, a cosmic ship will remain an artificial Earth satellite and will
describe an even greater elliptical orbit, the greater its velocity becomes.
The use of this energy reserve will enable a space ship to accomplish movement
around the ?arth in an orbtt,sclone to circular, located at varying distances
from the Firth.
Achieving a velocity in the range of approximately 11.5-16.3 kilometers
per second, a space ship can make flights to different planets of our solar
system; the ;rester the velocity of the upace ship, the more distant planets
it will be able to reach. Both the achievement of the first cosmic velocity
and of the other two critical cosmic velocities will be epochal in the history
of the development of mankind. It is natural that the significance of each
of these events will be all the ;reater, the bi,;,;er the mass of the payload
to which the critical speed is imparted. The impartin,; of critical velocities
to a payload of only several hilegrams has an imuediate symbolic si,;nificance
and speaks not only of an achievement of science and engineering, but also
of the limited possibilities for conductin;; the experiment.
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's'hun, the path of the J.'uture development of coamonuuticn is the otru~;t;le
l'ot' the mLtutery of Ureater pouni.ble velocitieo for the ;ventout, pouolblo pay-
lo-i. Pro,;reut, Ili tht.o utru,,,Je will be determined b;; the uuccanneu of rocket
oclcnac ai,d engineering, that Jo, It i.r1 1rooolbJ.e only on the bauio of further
Improvement and clove lopnient; of rocketu, rocket; et,?ineu, and 1'J.it;lrt control
oys Lem.;
To uo, i t; ncerns timely to or;;an t.ze the record in,; by an official inter-
nat lonu.l ors{arc of the ach l.ovcurcntu its the development of' rocket etu;ineorl nd
in the different, couritrle:;, jur;L an thin to be tar; done in aviation. The
recorded indexes should be the upced of 1'11t,ht, Lakin,; into account the
altitude and the mnl;nitude of the payload to which thin speed ii imparted
for various claoneu oi' rockets, (one-, two-, three-stare, etc.) and artificial
L'art'l- nutell l teo .
Peaceful competition of different countries in the rnantory of cuumic
opuco would L,rcatly utimulate the developmcw, of corirnonuutico.
The sunk. Lank is the further development of moans; ul' reachirl? conniic
,pace, that ii;, to develop the beat rocket ships.
The Line of rational layouts of rockets, ucienLil'i.cal.ly uubutuntiated
methods ui' cunr;truction, the moat durable and lil;ht cconntrucLion rnaterlalo,
and the creation of the want unproved control nyntemq, dint in.,uished for
exceedinl;ly Mill prec i c ion and moderate weight, will snake it pons ible to
achieve Successful results. The cevelopment of method, of computin,, the
most advuntu?eou:, t.rajcctories of the rocket in cosmic space and the render-
ing; oi' these calculutionu i'or concrete ?iven conditions it extremely impor-
tant.
The volume of computation work neccn nar;; In developing a apace ohip,
and ecpcciull,; fc.r :;elect;in rational f1i,;ht trajectoricn Is no vast that
cniy the une of hIL;1;-npeeJ electronic coomputern makes thin tank practically
solvable.
The letcrmltiln,; factor in ack'ornpli.nhiru; f1Jr;hts In cow:nlc ,pace is the
level of development oi' rocket en inc.w . The veluc i t,; achieved b,; a rocket,
in the i'irct inutunce, i:; determined b.; the power churacterintien of its
en;_ inc. In ccinte^rporar.i rocket en,;incr>. chenicul cnerr,:1 in used an a source
(if power. Further Irtproveirci,L of there er.;;ir,er; will rrake it ponnible ulti-
natel;; tc une 1'!il l,, %hc potent ial l t. les of chemical ,currc , of ener;;;; , with
the exIt velocity of the coirbu:,tirn product:: clo:;e to 4,OC0 rioter:; lie: necond.
Nultis%a,;e rccketc; with nu(-I, erk;iner, wit] be able to attain all three ccsmic
vela-cit.Icu, even when : tnrrL!t. , nrrn the :;urth, without udditicnal rcfuelitk;
at artificial :;aLelllLc:,. The une of artificial ::artl, natelliteu u:; an inter-
mediate land in; or refuel irk, :.tetion :cakes all corner:; of our solar nyutem
access lb le tc. rain, thus: .,uirantce i n,; the pone ib i l i t;; oi' fl iL;ht of :,pace ships
with ,rest pu;,ioudn.
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If we Lake into account the possibility of creating artificial Earth
naLclliteo as intermediate stations equipped with fuel reserves and other
rrkctcriala' near various planets, for example, Venus arid Mara, then it
becomes evident that rockets with en,;ines using chemical sources of energy
have already solved the problem of interplanetary communications.
However, the great distance of the planets, especially the outer over,
from the Earth means that a very long time will be require(] to reach theln
from the Earth, if the flights are to be made at velocities close to minimal.
For example, flight to the moon would take days, but a fl i l lI?i11; '.nl can ,,r di.n-
tiu;; i.L. 11rrr'erwr .?, tilt ()f the ;,od1rcr: l 11 _;ltt oi'-
I1c,I Vtrl to L ';,ii ' I lir, ' !"Lr! on Lh' a r'otir]ittun of tile'.
Lcopuuphr n, on Ito t.' ulrilr uc;; .
On the of trh:it 11-en been sacs:, it iu clt:u? that true outlined
and dint.'1.'iitiuli of in ~.odiaeal li, ht cannot be :.attained With-
out IL 1:no1;lcci, ;e of the eoefficiont of ti'rancip.u'Lnr, anti indicratrices of
csc,cttcr?i.cil; in t;c l'aaIkth'c; rat;,iO:plr'ii Lc .- 'rhel.c. The coefficient of
trantinarcnc;,? can ill,, dctertiiiird at ni;;ht, :nit thin iu not very eanily done
and rc hirer special inntr?iu:icnts. Indicat:icoo of scattering, another
important cier,iclit in atmocphrn-ic optics, can .ie accomplifhad only cinder
draylij;iit sour itioiia, when the In-i? htncou of the chy in determined only
by the ant ila.' distance from the Sun and by the -.cnith distimco from the
point of the: sky being; observed. Therefore, ohncrvations of :.odiucal
11L;ht for tlnr roc;;:ll,ilit; of making a complete reduction of the obcerva-
tions also rr?q'ti.-es .uldition.il data .-elated to the optical condition of
the atmosplieIa: .inch sho''.ld be L'.eten,iincd du,-in; the r'!ay with the aid of
approp: i ate :anpcar_atuc . Vo.' Vii., It Is accessary' to have two observing
parties -- one foo Bight, acid the otiie;? for daytii.ic o .rcervatiorit; and
their' i1c:;t _01:eui,icnt should !ic at a latitude of no more than ^lF?, that
is at the latitude of Asian.
It should also be noted that in southern ECZpt, atmospheric condi-
tions arc nca-ly ideal; as e. rule, clu"do are absent (occasionally there
arc cliL,_?*_ cirr~ is clouds)) and dust storms rarely occur. Humidity is very
low, '.?%? is b ?ightncs; of the day sky is formed almost solely by scatter-
in by molecules of air and fine dust. The absence of water
vair.'c in tic air over Ast:ran manifests itself also in a so-called phe-
nomenon of a Green :.-ay which may be observed, as a rule, each day during
sunrise or sunset and is distinguished by its very high intensity. In
addition, in the absence of clouds in the atmosphere, southern Egypt is
distinguished also by very high optical stability, which is very important
for the theoretical discussion of data obtained by observers. On account
of this, it is very desirable not to be limited only to minimally neces-
sary observations for discussion of observed data in relation to zodiacal
light but to formulate also a program of daytime observations related to
the optical properties of the atmosphere based on a very broad plan.
This is even more desirable, considering the fact that to this time
in Egypt, no observational works in the field of atmospheric optics were
conducted and available specialists were limited only to purely theoreti-
cal discussions, unconfirmed by factual data. On the basis of the ob-
servations mentioned in the program according to atmospheric optics,
problems having an independent interest were also included. According
to the facts mentioned above, the program of work of the expedition of
the Academy of Sciences USSR included the following:
CPYRGHT
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1. The conduct of general photometry of todiaeal light with differ-
ent light filters especially adapted for visual and photographic r4.gions
of the spect-ua. This photometry should be sufficient for constructing
a system of isophotes of zodiacal light taken separately for different
moments of time in the course of several hours of its visibility, right
up to the beginning of dawn, or immediately at the conclusion of twilight
and to a sufficient sinking of the sun beyond the horizon. All photo-
metric determinations should be expressed in absolute units, for example,
in the number of stars of fifth magnitude per square degree.
2. Determination of color of zodiacal light under these conditions.
3. Conduct of general photometry of the entire night sky, also in
absolute units. Appropriate observations can be conducted over very wide
intervals according to azimuth and zenith distance and should be suffi-
cient for making a system of isophotes of the entire celestial sphere for
each hour of time.
4. Special attention is paid to so-called pseudozodiacal light, the
zodiacal band and the Oegenschein.
5. Determination of polarization at various points of zodiacal " ght
situated not only on its axis but also at various distances from the paoane
of the ecliptic. The degree of polarization and the vector orientation of
polarization is found simultaneously.
6. Determination of the intensity of zodiacal light and adjacent
areas of the sky in separate emission lines, especially in the 55T7-
Angstrom line, in comparison with adjacent areas of the continuous spec-
trum. Determination of the increase of emission in different parts of
zodiacal light.
7. Photographing of zodiacal light with any kind of a camera noted
for very high ltght-gathering power, for example, with a Sonar/Zeiss ob-
jective lens. T'e photographs obtained should be calibrated with the aid
of an appropriate luml.nophore of known luminosity and should be suitable
for photographic measurements.
On the other hand, the program of daytime observations with respect
to optical properties of the Earth's atmosphere consisted of the lo'-lowing:
1. Systematic determinations of indicetrices of scattering by means
of measurements of the brightness of the day sky at different points of
the solar almucantar.
2. Determination of the transparency of the atmosphere for separate
moments of time according to a rapid method developed by Ye. P. Pyaskovekaya-
PeEenkova.
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3? Determination of the transparency of the atmosphere according
to ikn'guer's a!t.hod, end also according to the method of the solar aureole
ma.x IWAN.
4. Investigation of the change of atmospheric transparency during
each given day.
5? Determination of the polarisation of the day sky at various
points and its ,hange In specified points, for example. In the Zenith
during the day.
6. Finding numerical characteristics of optical stability of the
atmosphere, for example, in the zenith during the day.
Pr.paration for the Rxpedition
On the basis of what we said above, It is evident that observa-
tions of zodiacal light under the most favorable conditions should be con-
ducted vastest of all in the region of Aswan, Egypt, and particularly
during October-November, when the morning zodiacal light is nearly exactly
situated perpendicular to the horizon, and the evening zodiacal light can
also be seen very well, but rather considerably inclined. Parallel ob-
servations can be made in the U38B in the region of Alma-Atm.
The Comiittee for the International Geophysical Year under the
chairmanship of Academician I. P. Bardin approved my proposal in this con-
nection and petitioned the government to organize an expedition to Aswan,
Rgypt, under my leadership. The decision of the government was made on
26 May 1957. The staff of the expedition was compooed, in addition to
myself, of the following persons:
Ye. V. Pyaskovskays-Fee enkovs, Doctor of PhysIcomathematical
Sciences, head of the Division of Atmospheric Optics of the Astrophysics
Institute, Academy of Sciences Kazakh 88A. To bate, she has taken per-
sonal part is 14 different expeditions, several of which worked under
very difficult conditions, for example, in the Far taots,rn taiga, on the
desert of Sary Ishik Ottrau, in the region of dry winds near Pugachevska,
on Kuabel' Mountain, Tien-shan, and others. She has great experience as
an observer and has developed different methods !or determining the opti-
cal properties of the atmosphere, which have been presented in various
publications.
N. B. Divert, an Alpinist, a master of sports, also a participant
in many expeditions. He is especially interested in the phenomena of
zodiacal light and defended his candidate's dissertation on this problem.
Under his supervision an electropboto.eter for observing zodiacal light
was constructed.
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V. M. Kazarhevskiy, erientific associate of the Astrophysica
tnatittit., Candidate of Physicousathematieal $icienepg, head of the Chair
of f-,;rsies at Alma-Ata Medical Institute. Ilia dissertation concerned the
4$ffi"ult problem of photometry, determination of the albedo of the Barth
by the ashen light of the moon. Ile was also a participant in many expe-
ditions of the Astrnphysira Inst}tute of the Academy of Sciences Kazakh
MR and is a very close associate of Ye. V. Pyaskovekaya-Yosenkova.
P. N. ikoyko, junior scientific associate of the Astrophysics
tnatitute of the Academy of 8cienees Kazakh 880, who has taken part al-
raady in several previous expeditions of this institute. Ilia part in the
expedition to Egypt was to assist in observations, chiefly during daytime;
photographic work; and work on adjusting r"ed correcting electrical and
meehaniral equipment.
From the very beginning, as an essential condition to the success
of the expedition the partiri;wtion in the group of one of the Egyptian
astronomers, preferably from the Nelvan Observatory near Cairo, warn planned
L y us.
Instruueents of the Expedition
All instruments of the expedition a:e of original design, com-
pleted by associates of the Astrophysics Institute and for the most part
chocked for a long time under diverse expeditionary conditions.
In 1955, V. I. Moros, an associate at the institute, designed an
automatic elect rophotomete r for observing zodiacal light in the night sky
which was made in two copies by the Central Experimental Workshops of t':e
Academy of Sciences USSR. Considering this, it was decided to reject this
instrument which is more adapted to stationary conditions of operation.
In its place, in the workshop of the Astrophysics Institute, under the
Immediate observation of Divari, another electrophotometer was made which
was of simpler design and without automatic registration, but which oper-
ated on conventional batteries. However, this instrument, without fail,
required two people for its manipulation, one for the installation and
the other for readings of the mirror galvanometer.
This instrument is a vertical tube with appropriate optics di-
rected at the zenith. The receiving area of the photomultiplier, which
is always illuminated equally, is located in a Fabry pupil. The objective
lens of the instrument is directed at various points of the sky with the
aid of two large prisms with full internal reflection which are placed at
previously fixed intervals according to the azimuth and the vertical arc.
The cable connecting the photomultiplier with the amplifier and with the
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batte'ri?n In >>+aolutrl imthovai le. In the pror,'nrr, of an aaaintant, work
with this inr't.nlne'nt, proroerln Vrry rapidly said It reg1i1rc'n little time
for Nrth!F a ''1irtlot, '+f nhtiinerl rear'in n and foi their ,,nvpraion into
-vrrc,gjw A1nF; al anltit~' 1uminoniti"a.
()the- inatr'uir'ntn of the expedition, which have been well-rher?ke4
from their prevloun operation, included the following: A visual binocular
phntnnteter vi th merhani cal reitintration suitable for *ihotextietric work on
? 1I- sal li,-F,t, and alas for colcrimetr;,+ and polarization measurements.
11ie instrument is rrtnpleteiy portable and the comparison area in provided
by a luminophore of appropriate brif,htnean. A day sky photometer, also
of original deaiF;n, which has been used in many expeditions of the Astro-
ph;,aicn Inatttute. An aureole photometer of old dealft and a second
aureole phottwirter of new design of broken type. A theodolite for measur-
int-, Re~r:rap?sic ^oordinatea and determining the time, and vai loos auxiliary
small equipment. An ordinary Lcica, equipped with a EeisL Sonar f/1.5
lenn with r, focal length of rj centimeters, to used an a photographic cam-
era. Photographic film of very high sensitivity, namely 1173, was ouf-
ficient to obtain good photographs of zodiacal light with exposures of
only minutas.
In iddition to the scientific instruments designated for conduct-
ing obnervationn, the usual expeditionary equipment van supplied which
Might be needed under conditions of the Libyan Desert, such no various
mechanic;.l inatnunento. tents, awnings, white sun-reflecting awnings,
topot_;raphic umbrellas, sleeping l s, camp beds, camp tables, and chr.irs
and coarec felt blankets.
Further, various cooking utensils were taken, as well as office
supplien such an tracing paper, paper, journals for recording observations,
diaries, sketch books, graph paper, etc. Then, a fairly large assortment
of different nedicinen and, finally, food products -- oat flour, powdered
milk, rice, ounkwheat, bicculte, and sugar were also taken along. The
total wci,;ht of the entire expeditionary equipment, including scientific
instnunents, was nearlj a ton (9,V kiloaratns) and was cent from Alma-Ata
to Moscow, then to Odessa, an9 finally by sea on the steamship Pobeds to
Alexandria, E,;~rpt, with the understanding that it would be transferred to
Cairo to the address of our Embassy in the name of V. M. Kazachevckiy, a
participant in the expedition.
The expedition left for Egypt on the steamship Pobeda, which left
Odessa on 22 September. On 28 September, all members of the expedition
arrived in Cairo.
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Preparationn in Cairo of iiorpnsnry Conditions for the Work of the
Expp41ition in the Libyan Dpsprt in the Aswan Region
Prior to o'r departure to Alvan, it was absolutely necessary to
obtain appropriate orders from the variants Rpyptian authorities in Cairo,
with respect to the necessary aid at the working site. Professor Samaha,
director of the Helvan observatory, :ook a major part with us in these
tanks.
All members of the expedition visited Helwan Observatory and be-
came acquainted with the scientific workers and the scientific equipment
there. At this time, a polished and stained model of the Sikhote-Alinskiy
meteorite and various scientific literature were presented as a gift to
the Helwan Observatory from the Meteorite Commission of the Acedemy of
Sciences USSR.
According to an agreement with Cairo University and Professor
Saataha, the director of the Observatory, one of the astronomers of this
observatory, Dr Adli As'ad, was assigned to work with the staff of our
expedition. This was a great help to us and lightened our work in many
respects. Dr Adli As 'ad not only assisted N. B. Divari in all of his
observations with the electrophotometer but also acted as an Intermediary
between us and the population, taking part in all dealings of our expe-
dition with the various institutions and responsible persons, and he was
also a translator from English to Arabic when this became necessary.
To acquaint Egyptian scientists with the tasks of our expedition
and also with certain interesting investigations in the USSR bearing on
the theme* of the expedition, we delivered scientific papers in English
and in French. The papers were delivered at the Faculty of Sciences at
Cairo University, at flelwan Observatory, and in several other places. A
list of the papers read follows:
V. G. Fesenkov, On the Nature of Interplanetary Matter and on
Observations of Zodiacal Light (Faculty of Sciences of Cairo University).
V. G. Fesenkov -- Encounter of the Earth With a Minor Planet Pro-
ducing the Falling of the Sikhote-Alinskiy Meteorite (Faculty of Sciences).
Ye. V. Pyaskovekaya-Fesenkova, Rapid Methods for Determining
Atmospheric Transparency (Faculty of Sciences, Cairo University).
Ye. V. Pyaskovekaya-Fesenkova, On Certain Correlations of Bright-
ness of the Day Sky (Faculty of Sciences).
N. B. Divari, Twilight as a Method of Investigating the Upper
Atmospheric Layers (Faculty of Sciences).
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V . prrtr-ll:c,v, InventIf;fit ionn or Zo.I1ae r.1 Li.;ht and the Day
('ond+i- t.?-,1 in 1:x1W'dltIon of the Arfxdnrrt of, rlet+r(,n I1!lnll In Aswan
+1+11'll+F, O "tn+.n /:: ~VS'mlre" l'))'j (IIolpan n1~1:rrvitor;f) ?
Yr,. V. I`; f-al:ovr:l:~. '-->:cn~ nl:nvr', Certain Renultn i-'ith Ilrnpert to
Atoonpheri" Tr?incl+arc,nr.?;, Ind1 r'atrirrn of flratterint; and Pol ai i::ction ob-
talned In the l.il~;; an h^::^rt Itc:ar Antiutn in 0rtolior-ltovrmbe1' 1957 (ttelwan
01+nerv'tto)-;;) .
V. rl. Frnm-kov, Antronomliral Obaervatl.on During the Illy and f3ci-
entifir 3i;;ntficanrc of Artificial Earth Satellites (Soviet Embassy in
Cairo).
V. 'l. Fenenkov, nrowth of Ar tronomy in the USSI1 During the Pant
40 Yearn Aftc-- ttrc October Revolution (for ncientifie. associates and the
profcnnorir:.l ntaff of Cairo University).
In addition, on request of Radio Cairo, I delivered a speech in
French on the purposes of our visit in Egypt and on the artificial Earth
satel-liter. Lunched in the USSR.
Mcrrt,ers of the expedition had a number of possibilities for con-
tacts with Et;,ptian scientists. Certain leading scientists such as Pro-
fessor :t.,r:nad and Professor Madwar invited us to their homes; we met
others it special receptions which were given in honor of the arrival of
the expedition, namely by the Minister of Education; the President of the
National Committee on Scientific Research, Prof TLrki; and by the rector
of Cairo University.
I rreeived from the Egyptian authorities in Cairo the necessary
instructions uddrenced to the local governor in Aswan and to the head of
the Aswan Din with respect to the creation of the necessary conditions for
work in that place. After thin, on 10 October, N. D. Divari and Dr Adli
An'ad net out for Acwnn earlier than the rest of the staff of the expe-
dition with tici? clectrophotometer for finding a site suitable for ob-
cervationc and for finding proper livinG conditions for the entire expe-
dition.
After acvcral attempts, they finally found a completely suitable
area for ob cr?vationc, namely at the extension of the road being con-
str ucted throujh the desert to the now high Aswan Dam which, at this time,
is only being denij;ned. Great difficulty under Libyan Desert conditions
was found in grounding of electrical instruments. This Grounding was made
successful only by means of coupling the cable to an iron pipe which ran
from the Nile River a distance of several kilometers to the site where
the road construction work wan being conducted.
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In an area locaterl at a distance of approximately 20 kilometers
to the south of Aswan, rock r_oliunnn were built for the installation of
the tnatmunentn and also walls to protect them from wind and dust. Through
the r3overnor of Antran, a rent house located in a little village beside the
deem Itself on the right hank of the Nile wan obtained from the authority
of thn Aswan Brun. The rent house contained five living-roomn, including
a reception and dining room, two b:atht;, and kitchen and brad two servants,
a cook and military r;uard houncti in a military tent encampment around the
perimeter of the territory or the rent hobos and r'ontinuounly posted a
guard. Another Ovard was provided for oltr expedition on the territory of
the observation area itself and also wan quartered in a permanent military
tent enctunpment. As ft consequence, in the ol>rcrvation area, it was possi-
ble to place all of our equipment necessary for field work and to go there
for &baervationa only at specified hours of the day or nij;ht, whenever it
was most suitable. For this purpose, an automobile was assigned to as.
For travel to the observation site, it tas nerescury to pass the dam,
cross the Nil", and then travel around 1^ kilot,ictorn to the south to the
very end of the reconstructed road there the effect of city lights was
absolutely undetectable.
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Activity or the h;xpc'dit:on and rret.iminnry Results
Hegulnr observations wore begun by members or the expedition
ni"tnr 17 0s:tc%ber, , that is, after the ceacat ton or the light lunar nights.
To t.ho ar.pedition was nd4nd; on her own request, Dr Imarah tln'idah from
the University in Heliopol la , who wan interested in the works on atmos-
pheric optics and becatt the diligent assistant to Ye. V. Pyankovskaya-
Fesenkovn during her dnyt!me observations. This mai it possible to free
Boyko from assisting in Ye. V. Pyaskovskayn-Fen enkova's observations and
to detach him to photographic night work and partly to conduct observa-
tions with the aureole photometer alternately with Kazachevskiy. Daytime
observations can, in such a manner, be conducted in two shifts -- before
and after the middle period of the day, because for one and the same
observer it would be impossible to work under Libyan Desert conditions
when the temperature during the day rises to 450 centigrade and the sur-
rounding granite rocks freed from sand cover become intensely heated.
In such a way, participation of Dr Imarah in a certain degree
lightened the work or the expedition. In the interval between observa-
tions of Ye. V. Pyaskovakaya-Feeenkova. Dr Tmarah obtained for herself a
certain number of observat!.onal data with the day sky photometer.
The work routine of the expedition was as follows.
The day party, consisting of Ye. V. Fyaskovskaya-Fesenkova, Dr
Imarah Sa'idah; and Kazachevskly or Boyko, left for the observation area
at 0500 hours that is . even before s'.=.Ise -- so that they could begin
work at sunrise and conduct it continuously until 0900-0930 hours. By
this time, all significant atmospberi masses had already passed. The
second day party conducted observations usually only with the aureole
photometer to obtain data for the evening observations, which were con-
ducted by an observer who did not participate in the morning observations.
The evening party, consisting of Fesenk'va, Divari, and Dr Adli As'ad,
departed at sunset and remained until daybreak.. if the night was without
a Moon. If there was a Moon; it was poseable to leave later than sunset,
but Divari and Dr Adl:i As'ad always appeared at. the observation area at
least 2 hours before the actual beginning of observations in order to
switch on the batteries In good tame, permitting them to become stabilized.
The intensive heating of the batteries during the day, as a result of the
high temperature of the air; caused o convective flow within them and
disturbed the current stability. To store them at a sufficient depth to
protect them from the daytime heating was impossible because the entire
locality was composed of granite rocks wh.ch could only be blasted and
not chiseled.
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to general, working ronditions were rather difficult. chiefly as
result or the intense heat. and un-.wual drynena of the air and because
the personnel had insufficient sleep. The day party particularly experi-
enced difficult conditions.
As a result or the vf,rk, the following were obte tned:
i3inocuJar visual photcsneter (obrcrvrr Fesenkor) -- General pho'a,-
etry of zodiacal 1tgbf in the east aM wens. according to the program
mentioned abov*r lt."4y or ptleudi,zodlacal t 'RL6 ; and color rind polar.ttatton
at separato- points or zoc'tnca "l.:ght. The totAl n'ambo.r of determinations
or brightness for 23 ntght.e frost 18 October to 24 November wan 9,900-
N1Prtrophotc+srrter (obeervcra D)var! and Dr Adli Wad) ?-- rk,nernl
photometry, p'::+toaetric profile or th^ ertlre sky at different angular
die tances from the hor tz io .. d?term inati or- of r. of or . measurements of polar-
ization in the todtecsl 7lgth . an9 in the entire sky; and determinations
of the 1ntansity of the brightnesn iC the 5577 Angstrom emission line and
In the adjacent sect:('n of th' cont1w.oiu+ apectri of 5220 Angstrow
with the aid of an .. nt erfe rcnce filter. During t). nights;, from 19 Oct.o-
bar to 25 Nov ber 10, 300 A.etrrm+natiors of brightness were made..
Photometric camere 'observer Boyko! -- In the general complexity
of thlnae nr r-.'nd 50 phot.ographn of todiacal light., namely, its easternmost
rtgnt branch. were nwst
Day sky photometer !observer nyaskovakayn-Fesenkova, assistant
Dr marsh Sa' 4%,Ah -- Indicatrices of scattering, coefficient of trans-
parency; and polarization of the day sky at many points along the almuean-
tar of the s;u+ an1 continuously in the zenith The ?ot.al number of ob-
servations was a:o::nd 5,000, from 17 October to 22 November.
Aur-!o:e phctoroeter (K,azechevsk.i }- and Boyko es alternate observers)
-- From :.9 October to 22 November,, for 24 days , observations were made of
5 804 1,!tr'minat1.cns of bri&tness of the s'!reole around the Sam in pre-
noon and afternoon hours of each bright day..
Obeervntiona could not be conducted when the sky was covered with
cirrus clouds, which occurred frequently in November. One day, very dense
clouds completely covered the entire sky and the sun was not visible for
several house.
The n!-.ht sky in the Libyan Desert to the south of Aswan is not
distinguished by great darkness, and it is possible to see a great distance
and to photograph the surrcunding locality with a high-power objective
lens with exposures of around 15 m.rautee. In. spate of this,, the star
clouds of the Milky Way in a direction toward the center of the Galaxy de-
feat the Galaxy's brightness, which., of course occurs as a result of their
high position above the horizon..
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It is wonderful how the visiblu brightness of the zodiacal light
depends on its inclination to the horizon, how this is revealed in com-
parison with its west and east branches. On a night in October immediately
after twilight, the ecliptic is inclined 520 to the horizon approximately
at the amore angle as in the middle of August before sunrise in the region
of Alma-Ata. But zodiacal light is in a high degree weals and dim, spread-
ing to a considerable extent along the horizon in a northerly direction.
On the other hand, the eastern branch of zodiacal light reveals itself in
Aswan nearly normal to the horizon and far surpasses in brightness the
very visible part of the Milky May, at least in its parts c-.osost to the
Sun. This vast difference in brightness in the vest and east brancshe.s,
visible in the same night in Aswan, undoubtedly Is connected with the huge
increase of brightness of zodiacal light according to the closeness to
the sun. In addition to this, it should be noted that the eastern branch
of zodiacal light does not show the slightest propagc.tion in a northerly
direction; on the contrary, its northern contour is even more sharply
limited than the southern contour as a consequence of the presence in the
southern port of the sky of the Milky Way passing through the constella.-
tLri Monocerotis and, consequently, is more intensive in this region of
the sky of the gellactic component. As far as it is possible to lodge,,
scint5.llat-lon of stars in the Libyan Desert even near the horizon is very
small and the quality of pictures should be very good; however,, atmospheric
absorption near the horizon is undoubtedly great. Only such bright lights
As Jai. ter can be seen on the horizon itself immediately after its setting.
Stars of the first or second magnitude are revealed only at certain al.ti-
ttades. At the same time, the general atmospheric absorption is quite
smu.i1, particularly in view of the small height of the observation site
above sea level -- around 200 meters. The measurements of Ye. V.
Pyi+skovskeya-Fesenkova indicate that the coefficient of atmospheric trans-
p&rency in the Libyan Desert generally is no lees than in the mountain
regions of Alma-Ata at an altitude of around 1,500 meters. However, the
region of the sky near the horizon in our deserts -- for example, In the
Sary Isbik Ott.rau Desert near Lake Balkhash -- is more transparent than
in the region of Aswan. This difference is caused, evidently, by tropos -
pher,ic dust, which is more sharply expressed in the south of Egy;,t. Ob-
;;ervnt,on conditions would be even more satisfactory if it were possible
to fet? above this layer, being raised to a sufficiently high altitude.
Ye. V. Pyaskovskaya-Fesenkova found a number of interesting reg-
ularities Frith respect to the course of daytime transparency and degree
of polari:,at:ton., which will be discussed in detail in separate articles.
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Preliminary investigation of observation data leads to the fol-
lowing conclusions, the obser-rational aspect of zodiacal light depends
not only on the superposition of various sources of light rising out of
the upper layers of the atmosphere, out of the galactic component,, but
*o a certal.n extent also on the luminescence of the troposphere caused by
the zodiacal light ,itself. The observed but purely illusory stretching
of zodiacal light inclined to the North, which repeatedly was noted pre-
w1.ously0 depends in all probability on the zodiacal twilight caused also
by zodiacal light in itself., mainly its bright portions covered beyond
the horizon.
Polarization of zodiacal light decreases with angular distance
from the sun and is oriented, evidently,, precisely in the direction of
the Sun, at least in its normal position in relation to the horizon.
A review of photometric profiles conducted with the aid of an
electrophotometer In the region of the 5577-Angstrom emission line and
in the complex; region of the spectrum around 5,200 angstroms does not
ind.t.cate any ?rind of visible intensification of this emission line in
zodiacal light.
The inclination of the axis of zodiacal light from the ecliptic,
if it generally exists, should be absolutely insignificant.
The Clegenschein is slightly visible as a nearly circular dimmed
spot:, which at the end of October appeared in the vicinity of the Pleiades.
The zodiacal band was also excellently visible and cut across the whole
sky :Its brightness is comparable to the Milky Way in the region of con-
ste-11ation Monocerotis. It should be noted that around 0300 hours, when
thA Gegenschein passes into the western part of the sky and appears half-
way from the horizon, the lower part of the zodiacal band always is dis-
torted and produces the phenomenon of weak pseudozodiacal light which
was noted previously in the Sary Ishik Ottrau Desert on Tuyuk Su Glacier
and In other places. As the Oegenschein approaches the horizon., this
phenomenon becomes invisible.
Arriving in Aswan., the expedition maintained communications with
the Aswan authorities and Aswan society. Very frequently workers at the
Sam, the administrati.on,9 engineers, and even the director of the Aswan
Bank., who made our acquaintance, came as guests to our rest house. Twice
the governor:, accompanied by various officials, visited us. The governor
of Aswan gave a dinner in honor of our expedition and arranged a tour of
the :-arioua sites and a trip on a steamship on the Nile. The expedition,
on its slde., in connection with the 40th anniversary of the October Rev-
olution,, arranged a jubilee reception in a hotel in Aswan with a dinner
to which:, in addition to the governor, around 30 persons were invited.
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After dinner, a visit to so-called Kitchener Island was made.
An :Interesting botanical garden, which includes plants from all of Africa,
has been cultivated there in recent times. In general, our expedition
tiur lnrr its entire stay in Egypt appeared in a position as honored guests
an-1 was given the exclusive attention of the authorities and the popula-
t::on. All kinds of services were rendered us without charge -- the rest
house, the automobile, the benzene for it, the chauffeur, servafts, and
even the steamship. When the expedition desired to travel up the Nile,
transportation was provided free of charge for the entire day. The pro-
te.:t..:on assigned to us was actually necessary, especially at the observa-
t.ion area; without it, the members of the expedition themselves would
have had to continuously post a watch. At one time, our guards had co
fire on 100 attacking jackals., which surrounded us.
With the advent of the period of lunar nights, when observations
by night became impossible, the expedition in full complement vent to
Luxor, Karnak, and the Valley of the Kings and also visited the Coptic
Orthodox Monastery and certain villages in the vicinity of Luxor.
After departure from Aswan, on 26 November, the expedition made
a stopover in Qena. It twice crossed the Arabian Desert from Qena to the
shores of the Red Sea, and further to Hardek, near which is located the
well-known marine biological station. The expedition visited this station
and collected diverse information and data. On the return to Cairo, the
i xpedit :i.on during 1 1/2 days (4 and 5 December) ti Lveled, in an automobile
supplied by the Embassy, to the Suez Canal in Ismailia and further to Port
Se::d.; where it stayed over night. In the environs of Cairo and Aswan many
places, interesting in one or another respect, were visited by the expedi-
tion.
Finally, on 8 December, the expedition went from Cairo to Alexan-
dria, where the entire expeditionary cargo had previously been sent from
Aswan., We were successful-in putting the entire cargo, without delay,
on the steamship Pobeda, on which it was returned to Odessa. Three of
the members of the expedition returned to the Soviet Union on this steam-
ah..p The remaining two had flown much earlier to Prague on a.:. Swissair
plane, and then from Prague to Moscow on a TU-104.
The tasks of the expedition include not only conducting abserva-
t1or..s appropriate to the IGY program, but also establishing scientific
relations with Egyptian scientists, acquainting them with certain achieve-
rents of Soviet science, and adopting measures to permit the work on ob-
sarvations of zodiacal light, according to our program, to continue in
Egypt after our departure. Bearing this in mind, before our departure we
had foreseen the possibility of leaving our electrophotometer in Egypt on
r onrLLt~on. that the work of this instrument would be continued by the mem-
bers of the Helwan observatory.
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 The electrophotometer was transferred to the Helwan Observatory
In a special meeting in Helwan on 2 December, with the participation of
correspondents and representatives of the Soviet Embassy. N. F. Vino-
gradov, the Ifnbassy's first secretary for political. affairs, characterized
the arrivad of our expedition in Egypt and the transfer of the electro-
photometer to Helwan Observatory as a substantially real bond in the sci-
entific sense between the two countries. The Helwan Observatory proposed
to begin immediately the transfer of its magnetic division, which cannot
work well in Helwan because of magnetic disturbances. At the proper moment
our instrument can be set up at the meteorological station now in existence
in Fa,yum..
.Dr Adl. i A# ' ads who through many nights ass is ted Divari M t :U iu-
,i trunyent and becamde familiar with its operations can now continue its
operation independently, which of course is his own desire.
On 6 December, knowing; we were still in Cairo, Dr S. Hamid, also
from the staff of Helwan Observatory, told us that he r,Llso was interested
in th,to work and wished to take part in it.
During our stay in Aswan. Professor. Samaha, director of Helwan
Observatory, and Professor Hamad, head of the Chair of Applied Mathematics
at Cairo University, specially engaged in atmospheric optics, spent 3 days
with us.. They became acquainted in detail with the work of all of our ap-
paratus under field conditions at the observation area. Professor Hammad's
work has been purely theoretical and he is extremely interested in organ-
izing in Egypt regular observations on atmospheric optics.
In conclusion, I note that the expedition of the Academy of Sci-
ences USSR in Egypt for observing zodiacal light and the optical proper-
ties of the atmosphere was rather successful. All members of the expedi-
t?.on returned in good health. They collected a great amount of
observational material -- around 30,000 observations, which now should
be processed and discussed. They established very good relations with
Egyptian scientific circles and prepared conditions for future continua-
tion of our work in Egypt, with our instruments and according to our
program. They made many personal acquaintances, which may assist the
future development of cultural relations with Egyptian scientific circles.
[The report by Fesenkov is accompanied by a map showing the exact
locat'.on of the observation station outside of Aswan as being 23058.9'
North latitude and 32051.6' East longitude.] (Astronomicheskiy Zhurnal,
No 2, Mar/Apr 58, pp 305-313)
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Soviet Monthly Review Gives Cosmic Drita for October .157
Kosmicheckiye DannYYC (Cosmic Data ), No 10 (20)) 195'(p a monthly
review issued by NIZMIRcicutific Research Institute of Terrestrial
Magnetism, Ionosphere, and Radio Wave Propagation) of the Ministry of
Communications USSR, contains data for October 1957 of the results of ob-
servations on geophysical phenomena concerning; the electric and magnetic
state of the upper atmosphere: geomagnetic variations, the ionosphere,
cosmic rays, and earth currents.
The editorial board consists of the following members of NIZMIR:
N. P. Ben'kova, responsible editor and a Doctor of Phyaicomathematical
Sciences; T. S. Kerblay and Ye. S. Glokova, Candidates of Physicomath-
ematical Sciences; V. D. Davydov; N. V. Mednikova; L. G. Mansurova; 0. P.
Gorodnicheva; and B. S. Shapiro.
Information concerning solar activity and solar radio emissions
which were given earlier in Kosmicheskiye Dannyye in the form of tables
and diagrams are presented in abbreviated form solely for comparison
with geophysical data.
The table headings are given in both Russian and English.
According to this monthly review, the sharp increase of solar activ-
ity which began in June of 1957 continued in October. The activity was
comparatively equally distributed over the Sun's disk. The appearance
of new active foci of disturbances was noted. However the geoeffective-
ness of the active regions rarely declined. In contrast to September
1957, during which four periods of very strong magnetic atmospheric dis-
turbances were observed, October is characterized by a calm state of the
magnetic field and the ionosphere. In the beginning of the month, nega-
tive ionospheric disturbances were observed which were the end of the
very strong storm of the last of September. The magnetic disturbance was
completely ended in the first hours of 1 October. During the month it
is possible to single out 3 weakly disturbed periods:
10-15 October
From 6 October to 13 October, three active regions passed through
the central meridian. Region No 62, a steady active region in its last
revolution, produced an intensive magnetic-ionospheric disturbance. Dur-
ing the revolution, it decomposed; the active spot and flare area decreased
significantly. Chromospheric activity was still sufficiently high (3
flares were noted in the region), but the geoeffectiveness of the area
was considerably lessened. An extraordinarily stable active region in
the southern hemisphere No 63 (during the last revolution No 59), observed
on the 20th revolution of the Sun, continued disintegrating. Region 64,
a new growing active region, in its last revolution, presented its owr
separate spot. From regions 62 to 64, two of the small negative iono-
spheric disturbances and a small magnetic storm with a sudden beginning
(20382 on 13 October) were connected. Small disturbances with abrupt
beginnings (2038Z) were also observed in Earth currents.
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17-19 October
The 13-18 October stable active region No 65 (in the last revolu-
tion No 60) panned through the Central Meridian. In the southern hemi-
nphere during thin name time, a new, quickly developing region No (6 wan
observed. Both regions were almost nongeoeffective. Only two small
disturbances of short duration were observed in the ionosphere. The
magnetic field wan completely calm.
21-23 October
Small magnetic storms with unexpected beginning (2042Z) on
21 October) were connected with the stable active region No 67 (Central
Meridian 22-26 October). The first period of the storm wan characterized
by the great liveliness of elements which foretold the large storm. How-
ever, the storm did not develop. The amplitudes of the disturbance were
small. Similar disturbances were observed in Earth currents. (Kosmiche-
skiye Dannyye, No 10 (20), Oct 57, p 1-6)
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 Approved For Release 199p1Q8/08-CmR82AAq'OM7fQ00200270001-3
Amts Drift Station geverttyy iblyur-t
For the peat 3 months, the staff of 3evernyy P0lyus-7 has been con-
iucting scientific observations, according to plan, in the high latitudes
of the Central Arctic. On 1R Tune, Bevernyy Polyuc-7 cro4ped the 87th
degree northern latitude, and continued to drift toward the Beth degree.
All the work at the station is done according to the 1GY program in the
fields of oceanology, lonvApherp. serulr,vy.. mpt.ecrologyr, ani actinosptry,
as well 99 terrestrial magnetism. The work in the fl.dld of oceanology
has been considerably expanded over that of 1957, by Increasing the
amount of ice observations.
Severnyy Pblyia-l scientists have obtained new data in the study of
the b,t.tom relies of the Arctic Ocean. On 15 June, a new elevation of
the ocean bottom was discovered; the ocean depth at this place was ssarire
at 1..495 meters, while the surrounding level of the ocean bottom was 2,600
tr., 2.700 motors deep. The relative height of this elevation above the
surface >f the ocean bottom is 1,100 to 1,200 meter.. An analysis of all
previously mnaaared depths in this area shows that a now m.untain ranp
has been discovered which, according to existing data, is a spur of the
central arrt.ie elevation. The length of the mountain range is about 560
ki.:.rlnE Lore.
L r!ng the period of the drift, the station hat traveled over 150
mileN, however, on a straight line the distance is not more than 50 miles.
Ac,:nrding to preliminary data, the ice drift in the area of Severnyy
Polyup?'l is determined mainly by the direction of the wind.
In r:,nnect.ion with the unusually early summer of 1958, a heavy thaw
net in. Aa a result, large lakes of melt water were formed quickly,
v11ch r::raunded the station buildings. By taking the necessary pre-
caetione, it was possible to drain several thousand tons of water through
the station. -- N- Belov, chief of Severnyy Polyue-71 (Mbecvw. Vodayy
ranbpcz t . 1 Jul CPYRGHT
Oceaa tc Research in the Arctic
The 3c:'n c observations under a IU'r prcgrsm include a argil
amount ')f oceanographic research in the arctic seas. First of all,
observations were conducted in the Greenland Sea and the adjacent parts
of the Arctic Ocean, as a result of which valuable data were obtained on
the eater and ice exchange between the Central Arctic basin and the
reeniand Sea through the wide strait between Spitsbergen and Greenland.
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 Ap
rWbed FL~r~Fte sbi /Q 8-9bQ~9/4?~ stif hE~rR~P Q~1 0 A Q(,} 4.3,,,i s c t a n t i t t c
wt.or$el shoe that the edge of the iae pack has a-ivanced crynsiderably to
the nnrlh in the Greenlsnd Beim, and that a swell asrrint of ice vas being
rmrri.d -tit of the Control Arctic basin through the (lrgpnlend Goa. The
-cesnc rotphic work conduots4 In tt,e northern part of the (D aenland Bea
on t.ho On' and 1enn has confirmed the exlntencq of n deep Channel (up to
?,('ir swters deep) in the submarine elevation relied the "Nansen POrog"
in the conter of the strait between Greenland and Op:tabergen, which
playa an iMportAnt part in the vatar exchange t wean the North Atlantic
and the Central. Arctic basin.
The obaer,ation swterlols of t.hp station 'everWr Fnly.i .7, coll4cted
in toast of the little kn im reltiona of the Arctic Hied-. are also oxtrei mly
valAa!rlp. The drift, of thia station, in the direction of the Canadian
archipelago, is in keeping with the general ice conditions in marginal
erotic oean. eaet of Nnvocibirak.1ye Optrcrve. It definitely proves the
existence of a rlo e9 (:off) ice circulation in a clockwise direction,
In the part of the Arctic, Ocean adjoining the Pacific. This i.,e circula-
tion Is clcaely :onnpoted with the general atmospheric. circulation above
th! Central Arctic basin. -- A. Drelkin. chief of Divieton of Rcience
r in h ni atration of Northern See Route (ibrcov,
c nyy Transport, I . CPYRGHT
PpT 3 :sg 3r gxpelitton
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TI.,,!, trawler cgon', lead ship of the Pktriiug Sea scientific and fish-
irn; exp"ditiunr left Avschiralcaya Pukhte and needed for the ocean. In
an Interview with a Taos correspondent, Candidate of Technicel Sciences
V. -urdzyev, deputy chief of the expedition, stated that the main pirpose
of the expedt'lia was to study the distribution, accutrulatlon density,
and migration of fish, taking into account the oceanclogical condition.
Tbo Bering Sea region is comparatively new for fishing operations. This
rfg1,'4n viii nkv be explored for scien!ific ix rposes and at the same time
active 4.rsvling operations viii be organized. The scientific researeb
FhI i c be followed by fishing vessels.
The s.. entlate viii also gave a description of the sea voter, ctiirrents,
de4?1-sea fauna, and the composition and structure of the sea bottom.
Part )" the work is being done vithin the TCY program.
There hys never before been Ruch a large expediti' n in this extensive
r~-ginn ')f the Pacific basin. The expedition includes stout 30 baentists
of different s r:ialties.
.ofesb(-ra P. A. !bineyey. A. G. Knvnnevak!y_ nnM T. R_ Rna.?_ (at)n.?oy_
Vodnnyy Transport, 3 . ul 58)
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 pal rftedaFkKtReb AA9 OM&o fd 141 R000200270001-3
During the first 20 days of June 195f3, the average temperature
recordod at Komsomul'akeya was minus 67.5 degrees centigrade. At noon
of 17 Jun., an interesting phenomenon was obnerved for the first time.
Dearing a severe frost, the northern half of the firmsment, where the sun
was hidden behind the horizon, acquired a deep crimson color. At the
horizon the color changed over into bright yellow and in some places
into Qmorald. The whole range of colors, empecial.y near the horizon,
was iridescent and various shades intermingl.e-A. Such a phenomonon had
never been observed previously in the Arctic by any of the expedition
members .
Another unusual phenomenon observed by the antarctic expedition
members is the cracking of the snow surface under the influence of very
low temperatures. Cracks up to 3 centimeters wide and over 2 meters deep
are formed. The formation of these cracks is accompanied by loud noises
:eoembling thunderclaps or even explosions. Sometimes these "explosions"
are so strong that the station buildings tremble. At such times the in-
struments indicate marked the s in atmospheric pressure. -- Mikhail
Pokin, chief station Komsomol okays Hoeaow, Izvestiya, 3 Jul 5
CPYRGHT
pezrt. From Antarctic Station Pionerskaya
The Antarctic Station Pionerskays recently celebrated the 2-year
anniversary of its operation. This station is located in a :one where
the glacial "run-off" winds originate. During May, there was not a single
(lay without a snowstorm. The buildings of the settlement are connected
by subsnow passages and tunnels. In now places the ceilings of the huts
and the tunnel supports have caved in under the weight of the snow messes.
Now si %ppnrta had to, be built similar to those in rnkl ain'-a and arched
snow vaults were built above the ceilings to support heavy loads.
The snow dust, driven by strong winds, electrifies the antennas of
the radtc station, the instrument wires, and all the apparatuses of the
electromagnetic system. Sparks between the terminals of the radio receiver
and the antenna sometimes jump over a gap of 5 centimeters. During a
heav %e-nd, the men's electricity. -
Gri oriv S111n chief of station aka (hbscow, Izvestiya, 3 Jul
58) a CPYRGHT
0b' Returns to Antarctic
After leaving Chile, the Ob' headed again for the Antarctic, to the
Drake Strait. For 5 days, the members of the antarctic marine expedition
conducted research in this strait between Terra del Fuego and Antarctica.
Approved For Release 1999/09/08 : CIA-RDP82-00141R000200270001-3
 pproveddgr&igap61lAaWQ2/0i%ir ?C&-9?IA1 p2 J?RQ4e3grovn consider-
ably worse, but the work of the expedition vent on without interruptions.
On 10 June, the Ob' approached the southernmost point of the oceenologics
profile near Mordvinov Island (or Elephant Island), one of the South
Shetland Islands, discovered in 1821 by the Russian navigators F. F.
1411ingshausen and M. P. Ieaarev.
The biologists of the expeditions were able to do soar successful
trawling at this station, collecting valuable material from a depth of
400 meters, including various beaker-shaped glass sponges, rose-colored
hydrocorallinae, echinoidea, starfish, and other representatives of
antarctic fauna. The valuable specimens are being sorted and prepared
for nsaseumr by the biologists F. N. Pasternak and V. M. Koltun.
Professors A. P. Andriyashev and Yu. Ye. Pbrmdtin, the ichthyologist
of the expedition, have obtained for the first time on this trip large
specimens of a rare variety of "horned" white-blooded pike. These fish
of the family of white-blooded pike differ from all other types of fish
in that they have colorless blood, which has no red blood corpuscles
and hemoglobin whatsoever. AO analysis of the blood of these fish shows
that it is transparent, like water. Until now, these fish have presented
a mystery to scientists.
on, the Ob' will be on its homeward vgyagaj (IMbocow, Sovetskiy Flot,
Drake Strait as far a
From Mordvinov Island, the Ob' proceeded on 10 June in a northerly
direction, continuing to operate in the profile in the eastern part of
17 Jun 5b
- 31 - USCOUN-DC-5462
Approved For Release 1999/09/08 : CIA-RDP82-00141R000200270001-3