SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INFORMATION

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• Collection: General CIA Records
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• Release Decision: RIPPUB
• Original Classification: K
• Document Page Count: 17
• Document Creation Date: November 9, 2016
• Document Release Date: January 14, 1999
• Sequence Number: 1
• Publication Date: July 11, 1958
• Content Type: REPORT

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PR 131632-22
July 11, 1958
U. S. DEPARTMENT OF COMMERCE
Office of Technical Services
Published Weekly from February 14, 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 publications as indicated in parentheses. It is pub-
lished as an aid to United States Government research.
SOVIET BLOC INTERNATIONAL GEOPHYSICAL YEAR INPORMW ION
Table of Contents
I. Upper Atmosphere
II. Meteorology
III. Oceanography
IV. Arctic and Antarctic
Page
1
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I. UPPER ATMOSPHERE
soviet Program on Noctilucent Cloud Observations
In the first article of its kind, V. V,. Sharonov discussed the
Soviet program of observations on noctilucent clouds as follows:
In the program of observations which will be accomplished during
the IGY, observations and the study of a comparatively rare and very
little studied formation observed in the upper layers of the Earth's
atmosphere and known by the name of noctilucent clouds will be under-
taken
These clouds were discovered in 1885 in Moscow by the famous Rus-
sian astrophysicist, V. K. Tserasskiy, and independently by Iesse in
Germany. V. K. Tserasskiy, together with his young pupil, A. A. Belo-
poi'skiy, determined the altitude of these clouds, which they estimated
at approximately 80 kilometers. Thub was established an important fact
for the geophysicist, namely, the existence of the aerosol layers in the
upper levels of the Earth's stratosphere.
Subsequently, noctilucent clouds were observed and studied by many
scientists, and it was established that they are visible only during
twilight, only in summer, and only in a limited latitude zone, primarily
from 500-700, and also that their altitude fluctuates within narrow lim-
its from 80-85 kilometers with an average of 82 kilometers. However,
all of these works did not have any kind of systematic character, and
the results did not always embrace the desirable authenticity and ac-
curacy.
During the current IGY, for the first time, regular daily observa-
tions of noctilucent clouds by a network of stations and also by a series
of special investigations .on the principles of cooperation between a
number of scientific institutions according to a single plan have been
set.
In the USSR, the functions of the "main institutions" responsible
for the organization, collection, processing, and future use of completed
observations has been placed with the Astronomical Observatory at Lenin-
grad State University, where they will be concentrated in the Photometric
Laboratory. In the work on the study of noctilucent clouds, a number of
organizations will take part, including the hydrometeorological service,
where observations will be established at a network of stations; the All-
Union Astronomical and Geodetic Society, where work will be developed in
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is rnc.'l e.: Li;uated In a _;pecil'ico. iri.gh lar;itude zone; and certain oh-
rr,,ar;orier, Inaticute3, and others. For the coordination and se:ien;.:if:iC
ii ? rv i r.icrn of all of' these work:, ruder the interdepartmental conuni'ctee
:',; tho IGY, a special working group on noctilucent clouds has been or-
r!:,! Its membership :s of both as -ronomers and geophysic:iri;:
,.-n,rage:d in problems or the; upper atmosphere, as well as of experienced
c~~.)4; r ~Iers of noctilucent clouds. A. group, together with the All-'Jnion
A-2I.,uriomical and Geodetic Society, conducted two extended conferences
of ubrervers in Moscow, one on1 and 2 December 1956 and the other on
9 an'i 10 April. 1957. At these conferences, plans for investigating
r'.ocr J.ucerrt clouds by various :inst?itu ions arid organizations were beard
and confirmed. Also, instructions on obswrv'acions, which were subse-
quently printed and seat to all localities, were confirmed.
The Astronomical Observatory at Leningi ad State University set up
a special station for accomplishing its own program of observation.; and
for methodical work and the instruction of obsercrer's from other locali-?
1..ies,. This station is located in the city of Petrodvorets under the
Petergoi r.kiy Biological Institute of Leningrad State University. !'.s a
.eadquarters for the station, Building No 10, or "Naryshkinskiy Dvore.ts, "
which was destroyed during the war, was rebuilt. On its roof a brLck
.nvrzz was constructed, which makes it possible to see in the necessary
directions a perfectly open horizon. The organizer and chief of the
-,tar,ion is I. A. Parshin.
i'he basic task which should be solved by the observations complced
I
during The IGY is a prec-se establishment of the limits of appearance
of noctilucent clouds according to time and according to latitude. AL,
mentioned before, at presen?;. our information on this problem is based
on random and spurious material which in no way satisfies the require-
ment,s of scientific climatology. Suffice it to say that separate,re-
por'.; _: indicating the frequency of appearance of noctilucent clouds at
one o:' another station do not take into account even such an important
Jac'-.Dr as tropospheric cloudiness.
t:e USSR,, regular laily obser-trations of the appearance of noc:-?
i ilu Qc:. clouds are being c3nclucted 'by more than 200 stations within the
_,y, ;em of the Hydrometeorological Service (GMS) and also by volunteer
ob ,r i ,rers at stations organized 'by the branches of All-Jnion Ast_ronomi -
al and Geodetic Socie;;y. In the simplest case, observation is limited
ray t.rro e _?a'temeaU of the rrex'y fact of the presence or absence of noctilu'
c:en+, t:Louds within ,he limits of' range of' vision of the station during
;ne period of observation. At the same time, it is necessary to conduct,
a registration of tropospheric cloudiness as a fundamental factor de .e, -
m:ining The po,~sfnility or' impost?ibi.iity of seeing noctilucent clouds in
h.'r..e case of their presence. A more qualifying variation of observation
requires the fixation of the carve of the area occupied by no.rilzcen
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clouds in the sky, which is accomplished more easily by photographic
means, but; can be accomplished with the aid of the usual Theodolite.
A.~ far as the altitude of noctilucent clouds is concerned, this may
oe calculated by standard means. This makes it easy to obtain a
projection of the cloud cover over the Earth's surface. As supple-
mentary data, there are registered the visible brightness (the con-
trast with the background of sky) and the structure of the clouds
evaluated according to a special classification proposed by N. I.
Grishin..
A very important task is the regular, exact determination of the
altitude of the clouds. The most natural method is synchronous photo-
graphing from two sufficiently remote points and a subsequent process-
ing of the obtained negatives by photogrammetric methods. Generally
speaking, it is necessary to use a phototheodolite here because it is
necessary to have the elements of external orientation for the pictures
However, the use of phototheodolites in the practice of our topographic
organizations is rather limited,. --instruments of this type are not con-
structed by us. The other alternative is the use of aerial photographic
surveying cameras. Photographs turning to the horizon may be oriented
according to terrestrial objects, the altitude and azimuth of which is
determined by visual theodolite. For the sections of the celestial
sphere with a slight zenith distance, the reflections of the stars may
be used, but on pictures of the twilight sky, the latter is not always
obtained.
The problem on the most suitable direction of a base line is dis-
puta'`le. Some recommend placing it along a geographic parallel, refer-
ring to the fact that noctilucent c_i.ouds usually are visible on the
northern side of the horizon, in the specified direction, and with a
sufficient base line, the triangle will have the form, from a trigon-
ometric point of view of being the most suitable. Inasmuch as parallac-
tic displacement is directed according to the almucantar, the zenith
distances cut by the points of a cloud through both stations will be
roughly the same, which decreases the error connected with the inexact
calculation of differential refraction, as well as the systematic ef-
fects, depending on differences in the brightness of a twilight sky
background. However, these advantages may not be explained by the fact
...at, the structural details of the field of noctilucent clouds occa-
sionally have a character of threads and banks parallel to the horizon.
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'Jrdei the mea-;urement of parallax displacement,
'Jh , c'ri if.; also parallel to the horizon, will be very difficult. `There-
ru.ure., a more suitable direction of the bare line along the meridian is
},referred. In this ca;e, parallax displacement, roughly perpendicular
to t,he. :.iract1.irai parts, is mariii:'e_,-a?.ed and easily ineasured.
In view of insufficient clarity of the problem on the moat suit-
ible direc;ion of the base lime and the possibility of the appearance
of cloud; with a completely varied. structure, an entirely expedient
au.iggers r,i.ou should be considered to make ! i.mul ane-ous observations from
'.hree or a greater number of point,,;- Thus, the Sverdlovsk Branch of
the All-Union Astronomical and Geodetic Society plans to take photo-
graphs from nine points, the combination of which gives a base of
broad, long, and oblique directions. Observations from four points
are planned for Riga. Altitude determination will be made from Mos-
cow, Kiev, Kharkov, Saratov, Gor'kiy, and other stations.
The second very important task of precision photogramrnetry of
noca ilucent clouds consists of the investigation of their movement
a:Long the Earth's surface. It is known that such "drifting" of clouds
may occur with great epeed, usually exceeding 100 miles per second and
direction differing in various regions of the Earth. Accomplish?-
irkT, favorable photography of the area of noctilucent clouds from two
points, the displacement in space of individual prominent parts --
'lo+.s, crests, crossings of hail -- may be obtained. Great prospect3
are presented in this field for motion pictures, which have already
been used in the past with great. success in the work of the Geophysics
In,tir,~,te of the Academy of Sciences 'USSR.
Optical investigations of noctilucent clouds constitute a highly
impor,an,', but difficult problem. Their tank is to give material which
will make it possible .c draw a conclusion on he possible nature of
;he pari-.icles forming the cloud. It is desirable to determine the
following optical parameters: dis*:rib'i ion of tie scattering flow
according ;,o direction, i.e., ro-called indicatrices of dispersion;
change of the scattering abi _r.y wi".h long waves; degree and oriea.
tion of polarization., for light, sc.a".tered in clouds; absolute values
for the coefficient of dispersion for noctilucent clouds of various
.Ten-=i;.y; weakening of The ligi.itc of celes':;ial bodies observed through
a clcr?ad :-.over. In addi-,:ion, the opinion is expressed that the lumi-
nos ii.f of ;,Dct:ilucen-t clouds is de .ermined not only by the dispersion
of ,': e eun's rays, but also by he fluorescence of particles of a
under ' -e influence of ultraviolet or corpuscular radiation of
?e This brings up the -`.ask of searches of emission bands in
`:r,e .:i.oad spectrum and a more detailed study of their luminosity under
vari.o,as conditions of radiation.
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The fulfillment of the investigations enumerated above, coupled with
a number of difficulties, created by optical effects arising in the layer
of the Earth's atmosphere, are situated both below the level of the noc-
tilucent clouds, as well as above this level. Here are related the weak-
ening of the stream of the Sun's rays on their way to the clouds, the
weakening of the latter's brightness by its extinction in the layer, of
air lying between the cloud and the observer, and also the brightness of
the twilight sky imposed both on the visible picture of the clouds, as
well as seen through them. All of these effects must be calculated and
excluded from the brightness of the cloud finally obtained in the proper
way, which naturally presents its own extremely complex problem, espe-
cially if it is considered that noctilucent clouds are usually observed
at great zenith distances, and besides this, in a wide zone where there
is no basis to expect stable optical and atmospheric conditions.
Optical observations of noctilucent clouds are the principal task
of the Astronomical Observatory of Leningrad State University in Petrod-
vorts, and also of the expeditions organized by the Leningrad Branch of
the All-Union Astronomical and Geodetic Society by forces of students of
the Leningrad State University (a group of the latter is headed by 0.
Vas-il'yev, a student). Observations are also conducted in Moscow, Kalini
Tar*_a, and in other cities.
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The collective work for absolute photometry of clouds which is done
by stations located along the Moscow-Leningrad line of Ryazan', Perkhy-
shkovo (near Moscow), Kalinin, Bolgoye, and Petrodvorets is unique. At
the hour of day when the sun intersects the plane of the great circle
formed by this line, one and the same cloud is visible from all of the
points named, but at different zenith distances and, consequently, from
different directions. This makee it possible to construct an indicatrix
of scattering for the cloud particles. Naturally, the fulfillment of
such work requires clear weather along the whole line of the uniform
photometric system and of the careful exclusion of atmospheric influences
from the observations made in all of the stations. However, in principle,
the execution of such work is possible and therefore there is the expecta-
tion that in the case of the appearance of noctilucent clouds concurrent
with favorable meteorologleal tnnr1JtjnnP1_ i+ will 1-to --4%,l . I - ---.1 .1 --A I
(tlestnik Leningradsoga Universiteta, Seriya Matematiki, Mekhaniki i As-
tronomi, No 19, Issue 4, 1957, pp 184-187).
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r i oi i; - i': H cP1 Wor Lci 71,,,_'
1u-1 -ioar-;-i(:`1a..r ,Le 1 n tree World O)ceain, n
r.:. c, : c,-1~~ -per:i.od tide Of e won:i oeea)"1 re pr-: r;e,rt?s a two-node stand-
l n , 'Na c. , the )lode ; of are iocatccl in the vicinity of 30 degree,,,-
i"' 'o'.il.ii la'1: iLtud. , and the an.t:inodes 01 wi1'ich are at the eguat;or
rani i,'i ';'c-e polar rc:rions of tale sea. in i;?he equatorial region, the posi-
l, vc ar..cinalies of the values of the e.xci,;af,i.on force coincide with the
of ):re highest level of the Sea. In the polar regione, on
',.and., the positive anomalic-; of "tie excitation force coincide,
Jr. .r.?e~pec+, to tame, with the negative anomalies of the level. Observed
?a sti.a : confirm the conclusions of the theory of the long-period tide
i..iie C)t;ean,
.`;c.+ wave of the long??'perii.odtide is a forced wave, but 'rh e phases
):f T.' .' S wave do nct coincide 47L i.h the, vaiU.e of he force phase of ';';'he
Wa, e A lag of the pt:ase of the wave with respec'1? to the phase of thE:
for. ce inas been obierved. in the case of all the components of the waves
or ;r..: lore-period tide.. The average value of the difference between
`?` e 1e:L phase and the force phase has been found to be equal to plus
L ,:lays for the lunar semimonthly wave Mf, plus 1.9 days for the lunar-
:!olar semimonthly synodical wave P4f, plus 1.6 days for the lunar mori aiy
a e `4t;) , ai)F1 0..3 mouth for the solar semiannual wave Ssa. The average
val!ae for phase displacement for the semimonthly and monthly wave
of i, -.e long-period tide is therefore equal to 1.5 days. his is no-.;
expected, -ince G. Lamb (Gidrodinamika [HIydxcla.y!lamics], Moscow-
-,.rgrad i9 -7) already pointed out ire 'he dynamic theory of the long-
t. od tide that the deviation for this type of oscillation does not
,send Sole:Ly on. the dic'L~xbiiig force, + lie, pease displacements occur
i , ':w-yen ~ -~e o cMat- ions and their ctimulatir.g forces, dependY.r on
he frequeu:y cf:' he oscill.at{;:i.ons.
1i, wa-, found ';tat the size of the waves of the long-period tide in
Et L ;'OT.ISiC~..eTab .y F tCe~'1':; the 7?ze ? !.t?~C]pi3'ted for, these waves by
'.: e t;neory of the J'.orgVpe.rl_od i;ide. In the northern hemisphere,
'.)'' 2, r.e mos? coa?J'e.1ieift for oi;.iservations (between 40 and 60 degrees
nox tat, it-.;de j, 4:..e a-ierage -.value (average for 53 cases for semimonthly
and. no. ;hly waves and average for 86 cases of the solar semiannual wave)
of acnpli';udes of i.l,e ir.dividual waves of the long-period tide were
found ':o 1?' equal o 26.'4 m1.i. ime-vers for t-te Mf wave, 25.0 millimeters
fur P1S f wave , 32.5 millimeters for be Mm wave, and 39.3 millimeters
f":) c S`;a wave. Ti s means ';hat the semimonthly and monthly waves
o e ;:' E:r may -:l;nnge t n e a- ersge i?~,"'C:~ of he sea .her '168 millimeters in
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'enese latitudes. In the oceans of the high latitudes, this value. ob-
viousiy, becomes considerably higher. The static theory of the long-
period tide gives a value equal to only 34 millimeters for this char-
acteristic elevation of the combined semimonthly and. monthly tides.
Thus, the value of the actual long-period tide in the middle latitudes
is at least five times greater than the theoretical value.
The long-period tide in the world ocean is a force capable of in-
luencing the velocity of astronomical flow, thus effecting the circ,i-
a ono water and the drift of ice in the higher lntiturlpm (Dokiady
Akademii Nauk SSSR, Vol .118., No 5, 11 Feb 58, pp 888-890)
Use of Electronic Devices in Astrono Discussed by Soviet Scientist
In an article entitled "The Utilization of Electronic Methods in
Astrospectroscopy," N. F. Kuprevich, Candidate of Physicomathe,matical
Sciences (Pulkovo), discusses the use of electron-optical light con-
verters in combination with photographic plates by means of which the
effective power of modern telescopes and spectrographs was increased.
The image on the output screen of a converter proved to be con-
siderably brighter than a representation of it on a photocathode. This
ensures a gain in exposure, but) unfortunately, not in resolving power.
Recently, states Kuprevich, attempts using an electron converter
for photographing stellar spectra in the nearest infrared region were
made. For example, in the Canadian Astrophysical Observatory, a single-
stage converter was used for this purpose. The image of the infrared
region of the spectrum formed by a spectrograph in !ombination with a
telescope (reflector with a main mirror diameter of 180 centimeters),
was projected by the photocathode of an electron-optical converter.
Images of the spectra of the star d Bootes and 6 Ursa Major of
increased brightness obtained on the screen were photographed using
an auxiliary light-gathering optic on highly sensitive photoplates.'
During the photographing of these spectra in the 11,000 R range the
exposure was found to be 6.5 times shorter than in the case of direct
photographing of the spectra with the same apparatus but" without the
use of the convertor.
Experimental photographing of the spectrum of d Lyra during the
day in the infrared region of the spectrum was also conducted. Visible
in the spectrum obtained were Paschen series lines in the infrared re-
gion of the hydrogen spectrum, tellurd.c'bands (molecular), etc.
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Kuprevich states that the app ca a ono the television me d for
nteruJfy.i.ng the brightness of :image,; in astronomy in general anc in
:~'.ellar spectroscopy in pax ,icu.lar promises great prospects. Un r-
7unately, the conventional elev:ivion transmission tube of "supe rthi-
con" type possesses compar ivel.y little sensitivity. These tub sys-
tems cannot store energy iT the image over a long time. In TV t ns-
mitting tubes, the superor icon included, the image is accumula d in
the form of electrical char es on their targets. The usual stor e
time is 1/25 second.
Recent e.cperiments in 'alifornia on the possibilities.of in easing
the storage time of images n the superorthicon, that is, of ins asing
Its sensitivity are mentioned by Kuprevich. In these, the storaE E! time
was successfully brought u to 20 minutes and more. In achieve this,
it was found necessary to 1 duce the voltage in the photocathode tube
from 500 to 50 volts, to c 4l the tube down to a temperature of 11 0 de-
grees, to decrease the cur nt of the electron scanning beam in e tube,
.and to increase the scanni time up to 5 seconds.
A similar "cooled sup_ orthicon.." obviously can be used in p tomet?ry
of the solar spectrum, conc udes Kuprevich, and it is certain th
agplinn-tAnn osc will also e very effective .(Priroda,
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Soviet Scientist summarizes Some Results of Upper Atmos re Rocket
Studies
V. V. Mikhnevich, Candidate of Physicomathematical Sciences at the
Institute of Applied Geophysics, Academy of Sciences USSR (Moscow),
gives Some Results of Investigations of the Upper Atmosphere," which
appeared in a popular science periodical of the Academy of Sciences
USSR, as follows:
"The study of the structure of the Earth's atmosphere; of the
ultraviolet, X-ray, and corpuscular radiation of the Sun, acid of the
illumination of the day and night sky enters into the IGY program. The
structure and composition of the ionosphere, terrestrial magnetism, and
meteors and micrometeors are also studied.
"Rocket investigations, aiding in the study of the physical regu-
larities and processes arising in the upper layers of the atmosphere,
and solar radiation and its effect in the Earth's atmosphere occupy an
important place in the ablution of these problems.
"The weight and the height to which scientific apparatus has been
lifted into the upper layers of the atmosphere have been increased coh-
siderably of late. In the first vertical rocket launchings in the USSR
in 1949, the atmosphere was probed up to altitudes rf 110 kilometers,
At this time the weight of the scientific apparatus lofted did not excee
120-130 kilograms. Owing to the creation of powerful geophysical rocket
in the Soviet Union, the ceiling of the investigations in vertical
launchings has considerably increased. In 1957 rockets with scientific
apparatus reached an altitude of 212 kilometers, and on 21 February 1958
had already gone to an altitude of 473 kilometers.
The scientific program in the last rocket launchings was consider-
erably expanded. In the first rocket investigations the structure of
the atmosphere (pressure, density, temperature, composition of the air,
and the velocity and direction of the wind) and the intensity of cosmic
radiation were studied. Now, in addition, studied of the ionosphere,
solar radiation, the motion of meteors, etc., are conducted,
"A wide variety of scientific apparatus was installed in the rocket.
"The concentration of electrons in the different regions of the
atmosphere was measured with the aid of a dispersion interferometer.
The temperature of electrons was determined, using special sondes, by
a method of sounding characteristics. The ion composition of rarefied
gases was established by a radio-frequency mass-spectrometer, and the
concentration of positive ions was measured by ion traps located on the
rocket's surface.
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 ;on_zatinn and mag ie: ir. a .ncnn ,e. a gavc in-{'ormutJ.un on the pressure
of the air.
"The energy and number of micrometeors was registered by special
piezoelectric transducero, The ir.';,c,ns ty- of the electrical field on
the rocket's surface was mesa ured by special dynamic electrometers.
"In some launchings a spectrometer was in: tilled in the rocket which
made it possible to photograph the solar spectrum in the short-wave
ultraviolet region.
"Particularly interesting results were obtained during the flight
of the rocket on 21 February 1958 up to an altitude of 473 kilometers,t,
"The flight of 'the rocket was :stabilized.. This is essential for a
whole series of experiments.
The totalweightof the scientific Instcr?.anents, the radiotelemetering
apparatus, the power sources, and the auxiliary systems together with
the structure of the instrument container was 1,520 kilograms.
"This ascent, as to both the extent of the scientific program and.
the altitude achieved, exceeds investJ.gations of the upper layers of the
atmosphere previously conducted. in the DER and. abroad in vertical rocket
la.ur..chings.
"As a result of the investlgat1ons conducted, first of all a whole
new range of information concerning the upper atmosphere was obtained..
Thus, the measurement of electron concentration showed that, in cont:ast
to earlier assumptions, there is no sharply expressed ionospheric layer
at. an altitude of 110-120 kilometers; the electron concentration above
110-120 kilometers decreases 1r.~sig1:.J~'Jct,.ratly and increases evenly to an
elti'cud.e of 250-300 kilome:te=s. Aybove the ma.ximi:sn, located at an altitude
of about 30G kilometers, t'h of electrons decreased slowly
so that at an altitude of +7O kilometers the electron concentration equaled
one million electrons per c llc c~W?';. mecec. This was shown by recent, n-
ves;;igation by the Soviet, geophysical roc et.
"It
"It should be note,: t:?mt ome-,r_i...E.;.. , 5.-rives t iga~ ions (Bern?ing), conducted
up 'co altitudes of 380 1cJ.lorlP;;r.1?s, s.:7e in conflict with these recent
results. Acccrdinr to thneeir de. n, concentration is already
negligible at an a=..tiuude of 3-0 .'? _oiue: tiers .
The existence ~o~r. lar1g conce.,,,7.:ration_e of electrons at altitudes of
1, 4 11`Jme t~~~i?J, YI/ crc ~lhe .?'S. c`-:it a ton of neutral particles is ap-
proximately on the o ?der of 1& ge elect-on concentration, may be explained
by the intensive diffusion of electrons from the underlying region of
the ionosphere.
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"1.'i1o eritablishmcrtt of the Pict; hail 7-.c 100 k:i.1_ometcre, there is no
di.t.fl.'?.wicm sepnrrttion is r:no1;her i';andarncn~;c.1 resu:i.t of rocket investiga-?
Lion:?;. This was determined by '.-.he, ,_analyr:is of air arnplcs taken by
special balloons at a1.t ituder; oi' up ;o 120 kllome';ers. The ion com-
position of at;moapheric air up to nititud.es of 206 kilometers was deter-
mined with the aid of the
rnacs -~~pec; rome;,r.r.
' asuremcnts of the energy n.nd number of meteor particles makes it
possible to obtain the dirtr~ibu-,;i.on of m:Lcroparticles according to al-
titude. In the 21 February experiment the impingement of particles tip
to altitudes of 300 k'_lomcter:? was reliably registcied.
":To :Lesa interesting data were ob wtincd in regard to the pressure
and derwity of the upper ai;mosphe:?e. Ttie greatest altitude to which
measurements of pressure were cunductei, 260 kilometers, was achi.;ved
during rocket i., ies t igat ionu in the USSR.
"Investigations of the upper rtro,3phere with the aid of vertical
launchings of rockets and artificial earth satellites, which are planned
according to the 1.?G.'. progruin, matte it pos7-i:ble to improve the accuracy of
4-.ho F ob-L%ain new antra. on
the prccesses takinj4 place in i:." (Prirodn.; No 5, May 58) pp 71-72)
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Solar Activity and Atmoolip erir. C'_i?.^. ,1 ~~atio;z'
"Certair. Hypotheses on the C_;nnert:?un c,i' Solar Activity With
Atmospheric Circulation," by A. A. Ihn:'.;riy~ , appearad in. Solnec_ e
Da e, No 1, 1957, PP 153-159.
Taking as a basis one of the carliebt; h;hpotheaes concerning the
physical co xiectluu of solar atmospheric circulation, the
so-called condensation theory, Ibni';.riyev propo,-,es that an increase in
solar activity is a.scmpanied by -a increase in the number of condensa-
tion nuclei in the atmosphere by thr. s.e ,.i.on of ull;raviolet radiation and,
therefore, more favorable (:on ition. f ,r ;re r.-?lease of the energy of un-
stable moisture content.
The data of come 1abora.to:.y e: ;eriments and rocket ascents confi.4?m-
ing this theory are give:.-, by 's',ic ;author.
ri'heoretical invest i ation:, e.:gg1 .i'a.irg the roir_ oy strong fluctuations
of circulation in the upper tropor;phere were conducted. These showed
that the effect of variations of velocity even at twice the altitude of
the tropopause and at near tropopeuse veloci?tf were negligible.
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During, investigations of the mechanism of the process of convection
by rotating models as it applies to the atmosphere, the predominance of
cyclonic circulation near the Earth with an increase of temperature in
the upper layers of the atmosphere through their more intensive irrndia-
tion by ultraviolet rays was established.
Dmitriyev concludes by saying that the fact, noted in literature,
of the change of zonal circulation during fluctuations of solar activity
leads to radical expansions of the gaseous envelope of the atmosphere.
(Referativnyy Zhurnal -- Geofizika, No 2, Feb 58, Abstract No 1129, by
G. I. Morskoy)
Results of Seismic-Acoustic Studies of Bottom of Japan Sea
The results of seismic-acoustic investigations in the western part
of the Sea of Japan, which were conducted in April 1957 by an oceano-
graphic expedition aboard the Soviet ship Vityaz", are given in an article
by N. N. Sysoyev, G. B. Udintsev, and I. B. Andreyeva, Institute of
Oceanology, Academy of 'Sciences USSR, and the Acoustics Institute,
Academy of Sciences USSR.
The studies were conducted along two mutually perpendicular profiles,
located in the transition zone between the Asiatic continent and the bed
of the Pacific Ocean. One profile ran approximately northwest to south-
east, transverse to the continental shelf, and the other from northeast
to southwest along the strike. This location was chosen with the aim
of shcwing the conditions of seismic wave propagation in relation to the
structure of the continental slope, and in particular to the presence of
supposed discontinuous dislocations.
The method used in the operations was, basically, the reception and
analysis of reflected and refracted sound waves spreading in the mass
of water and the porous sedimentation and rock lying at the botton of
the sea. The work was conducted from two ships -- one setting off charges
of TNT at fixed intervals of time, and the other (the 'Jityaz') lying at
drift at the beginning of the profile receiving the acoustical signals
of the explosions using hydrophones. The profiles were worked in both
directions.
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The data oht.at.ned indicated the presence of very thick depositions
In 1-