SCIENTIFIC ABSTRACT LYUBIMOV, G.P. - LYUBIMOV, L.A.

• Document Type: CREST
• Collection: Scientific Abstracts
• Document Number (FOIA) /ESDN (CREST): CIA-RDP86-00513R001031210009-4
• Release Decision: RIF
• Original Classification: S
• Document Page Count: 100
• Document Creation Date: November 2, 2016
• Document Release Date: August 31, 2001
• Sequence Number: 9
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

12
On the Polarization of a Molecular Be-Im by ar; Alter-na-, e--- ';i r:@
Amplitude and Phase
the actin.,@ 'ield clian-e slo@aly.
4.) Discussion of the c@tse in which the a,--.@Flitude requency of
the acting field chan6e rapidly.
For the case that the actin@., field wit': chan,@in@,, corre-
sponds to the frequency of a molecular transition, an @!xact j(,lu-
tion of equations was derived for poLirization. For thf! case that
the amplitude and frequency of the field cha.@@-e 31owly r
an approximate solution is .,-.iven for the (,-,t,ation.
There are 4 Slavic refer@:nces.
AS-'@OCIATION: Moscow State University
(Idoskovskiy Eosudarstvennyy universitet)
SUBMI17 ED: May 2C, 1957
AVAILABLE: Library of Congress
Card 2/2

AUTHORS: rx'vozdover, 3.D., KQ
TITLE, Experimental of Ui! @D
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AUTHORS: Lyubimov, G. P., Strakhovskiy, G. M., Cheremiskin, 1. V.
TITLE: Simple method of tuning a molecular generator
PERIODICAL: Vestnik Moskovskogo universiteta. Seriya 3, fizika,
astronomiya, no. 1, 1961, 79-81
TEXT: At the B&oskovskiy gosudarstvennyy universitet (Moscow State
University), a molecular generator was produced and put into operation
in 1958, whic@. operates with the lines I - 3 and K - 3 of N14H3 and
corresponds to a type developed at the FIAN by N. G. Basov and
A. M. Prokhorov (Ref. 1: Basov, N. G., Prokhorov, A. M., ZhETF, 27,
431, 1954; Ref. 2: Basov, N. G., Prokhorov, A. M., DAN, 101, 47, 1955:
Ref. 3: Basov, H. G., "Radiotekhnika i elektronika", 1, 752, 1956). The
molecular beam was formed in this molecular generator with a Cu-foil
grid having square holes with a lateral length of 0.05 mm and a duty factor
of 0.25. The authors studiod a roplacoment of the grid by a single channel
10 mm long with various diameters. Optimum results were obtained with a
channel 1.5 mm in diametert as compared with the grid type, the sig-nal-to-
Card 1/4,

12- -1) 1
S/188/61/000/001/0,30,1/009
Simple method :)f tuning a .... B104/B203
noise ratio coild be increased by the 2-5 fold. The signal-to-noise ratio
was 20-30 db. Further, a simple method for the start-up and coarse adjust-
ment was suggested. The principal stages of the start-up of tho molecular
generator are: tuning of the resonator for the absorption line, observa-
tion of the induced emission and generation, tuning of the resonator for
the spectral line. In general, the transition from one stage to another is
connected with changes in the radio circuit. The method suggested does not
require any changes in the radio circuit, and permits a quick start of the
molecular generator and a quick adjustment for the frequency of the spectral
line with sufficient accuracy. Fig. 1 shows a block diagram of the arrange-
ment, While the switch is closed, a saw-tooth voltage of a few kilocycles
is applied to the auxiliary klystron of the "intensity gate", & frequency
characteristic is observed on oscilloscopes, which consists of a number of
narrow vertical lines each of which is a resonance curve of the narrow-
band intermediate-frequency amplifier (band width 50-100 kc/sec). If the
resonator is filled with ammonia at a pressure of 10-2_10-4 mm Hg, the
frequency characteristic of the resonator shows a trough due to ammonia
absorption. In photo.-raphs of the oscilloscope trace, the absorption line
is observed ul to pressures of a few lo-5 mm Hg. With higher vacuum and
Card 2/@

@ 1-f- -L4
S/18 61/000/0o1/009/0o9
Simple method of tuning a ... B104YB203
application of a voltage to the sorting system, the trough caused by
absorption disappears, and an ejection appears instead of th2 absorption
line; the ejection is caused by the initially induced emission and also
by the gene:,ation. The tuning of the resonator adjusts the 2'eneration
line to the maximum of the resonance curve of the resonator with sufficient
accuracy. @fter switching off the high-frequency savi-tooth roltage, the
signal of the molecular generator is obtained on the oscilloncope. There
are 4 figur,.-s and 3 Soviet-bloc references.
ASSOCIATION: Kafeera atomney fiziki (Department of Atomic Physics)
SUBIMITTED-. July 18, 1960 Ix
Card 3/4

ACCESSION N'@: AP4043502 ~/fj293/64/(jo2/(jO4/0633/CJ64(i
AUTHOR: Vernov, S. N.; Chudakov, A, Ye.-, Vakul0v, P. V.; (;orchakov,
Ye. V.; Logachev, Yu. I.; Lvuhimov, f,. P.; Nikolavev, A. r.
TITLE: Investigation of cosmic radiation during the flij,,ht of the
Mars-1 and Moon-4 space s'ations
SOURCE: Kasmicheskive is;lednvaniva, v. 2, no. 4, 1964, 633-640
TOPIC TAGS: cosmic radiation, space station, Mars 1, '!oon 4, Earth
radiation ttelLj scintillation counter, gas discharge counter
ABSTRACT: Recordings of cosmic-radiation intensitv beyond the Earth's
magnetic f Leld made during the f light3 of Ma rs-1 (20 Novemher 1962 to
25 January 1963) and Moon-4 (2-14 April 1963) are discussed. Data on
the Earth's radiation belts received f rom Mars-1 and data on
the cosmic-rav intersity during various cycles of so:.ar activity
are given. The equipment aboard Mars-I consisted of two scintillation
and two Geiger gas-discharge counters. It was discover-ad that the
intensity of cosmic radiation remains practically constant beyond a
distance of 0.24 astronomical units. During the flight of Moon-4,
Card I / 2

ACCESSION NR; AP4043502
slow and smooti variations in cosmic-rav intensity connected with
changes of the magnetic situation in the solar system were recorded.
The particle fLuxes in the radiation belts recorded by Mars-I
are given. The average energy yield in the crystal of the scintil-
lation counter!; for a single count was about 2 Kev. Orig. art. has:
5 figures and it tables.
C,rc: 2/2

r s
L 21116-!@5 ~l:-C-4/~".]G(v)/k-.WA(h)/E7,iT(1)/FEC(t)/FS(l)-3/EEC(m)/r-CC/FSF(h
Pe7 -57P-g-4/Pi-@/PJ-4/po-41 Pq-4/Pa a -2/Peb/Pb-4 AEDG(b)/BSD/AF'~iL/SSD/AliD(a)-5/
A--'DC(a)/AFI-ID(C)/Ay--Ttl/AF-IG(a)/AFTC(b)/APGC(f)/F~'D(Bi) TT/GWAfS
ACCESSION NRS AP5002106 5/0048/64/028/012/2058/2074
AUTHOR: Ve-rnq, v-, S. N.; Chudakov,_!@,_jej Yakulo.y, P.. V.1 Gorchakov.-IL
-ye, V.; Ign4t'yev P. P.; Kutnetsov. 5, N.; Logachav. Yu. 1. Lyu@Amoj@,_
I 77-0khtopk9y V, F . 0 &-
N i ro-Ta y a v Solnovets, 5 N. I rAft*v,#WaYi
V"
TITLES Radiation study by Cosmos I [Report presented at the Vae-
soyuzaoye sov4shchaniye po fLzLks koamicha#kLkh luchey (All-UnLon
Conference on the Physics of Cosmic Rays), hold at Moscow. 4-10 Oct-
ober 1963]
'SOURCES AN SGSR. IzveacLys. SerLya ftst,cheskays, v. 28, no. 12,
1:1964, 2058-2074
TOPIC TAGSt radiation measurement, spaceborne iouLzatLon measuramenC.
n
primary cosmic radiation. se. in iLlat on unter,
_-.. _;@ --------- i -An- gas discharge count-ort
STS-5 gas discharge counter, Cosmos-17
ABSTRACTS The article describes equipment used in the flight of
Cosmos-17 (apogee, 788 ku; perigee, 260- ka) for investigating the
Earth's radiation belts and primary cosmic radiation.. The equipment
consisted of two scintillation counters (with Hot and Cal crystals) aad
Card

L 21116-65
ACCESSION NRI AP5002106
a STS-5 gas-discharge counter. The cylindrical Rdl counter (20 X 20 as)
was mounted uti,der the shell of the satellite and was fitted with
aluminum shielding (l 5/CM2). On one channel it recorded Ionization
produced in the crystal by radiation,, on the two others* it regia,:srsd
the number of pulses with energy release In the crystal over the
specified throsholds (50 key and ?fay). The effective cross
section of tho Nal crystal for particles registered along th4 Loniza--
@t ion and'.first threshold channels was approx..4.7 cm2; for the socoad,
channel, it w,ia roughly 5% smaller for particles with quadruple ioni-
zation and 20:9 smaller for relativistic particles.
The STS-5 gae-discharge counter has an effective cross section of
4.3 cm2. It was placed inside the device containing the scLatLILation
counter and was not fitted with any special protection. Up to cauot-;
ing rates of 3 x 103 pulse/see, the counter registered virtuall:p all'
particles. At higher rats4 the iount became loss reliable.
The flat CsI counte.(crystal diameter, 6 not thL0a4ss, 3 no) was
mounted oucside the container. For,;Vocertti,oa from light, the crystal-.-
was covered with aluaLaus fail (2 a cal). For protectLoa &SaLost
Card 2/5

L 21u6_65
ACUSSION HAs AP5002106
byemastrahlung. the photomultiplier and the crystal were shielded
with 5 mm of lead and 11 mm of aluminum, except for the front of tile
photomultiplier. which had a conical opening for particle iacidenc@s
(aperture angle, 40*). This counter carried out ionization measure-
ments and particle registration at energy release in the crystal of
45 and 160 kew and 5.4 and 8.5 Mev.. Both electrons and protons could
be registered along the first two (45 and 160 Kov) channels. Along
the other two (!i.4 one, 8.5 Fav) channels, the count was mainly of pro-
tons; at an ola,:tron path perpendicular to the cryst&l surfacer snarxy
Vonsos vQra*abo,it 2-11sv'ind oblique-paths were.*Vzooludild by:;he chick-
nose of the shielding.' Table I of the Znclosure gtvas the minimal.'tio
partL@la aounters.,_Orig.;&rt.Ih&sI-Z I
tables and'4-formul4d;.
ASSOCIATIONs none
Card 3/5---

P@,'c-3-67 JK'f
ACC NR. AP6030010 SOURCE CODE: UR/0020/66/1,59/005/10"/1047
AUTHOR: Vernov, S. N. (Corresponding member AN SSSR); Vakulov, P. V.; Garchakoy, Ye. -V.;
Logachev. Yu. I.; Lyubiiov, G. P.; Nikola ev A. G.; Pereslegina, N. V.
ORG:
Stu
TITLE: Measurement of intensity of penetrating radiation on the Moon face@
[Paper presented at the Seventh COSPAR. Meeting held in Vienna in May 1966-1
SOURCE: AN SSSR. Dokla y, v. lZ9, o.
TOPIC TAGS: moon, radiation intensity, lunar probe, radiation measur0ment/
Luna-9 lunar probe
ABSTRACT: The lunar probe '11!!@ @a- launched by the So,riet Union on 30 January 1966
made a soft landing on the Moon on 3 February at 24 hr, 45 min, 30 sec
(Moscow time); it was equipped with an instrument containing a 6 x 10-rnm
discharge counter to measure the intensity of radiation. The minimum
shielding of the counter mounted inside the probe near its jacket was -l gm/cm2.
The instrument was, switched on immediately after "Luna-9" was put
into orbit and was kept in operation until the probq,@topped functioning. The
data on the intensity detected with the as counter\ averaged over 14 time
intervals are shown in Fig. 1. The first five time intervals are those for the
flight from the Earth to the
Lcard

ACC-NR.
count/sec
'rime of
land ing
Measurements diriM Measurements
the flight to the Moon on the Moon
I I I I
311 Iff 2ff 3ff UIT Y It )968a
Moon. The next (sixth) int,-rval
is that for the flight near the
Moon (beginning with at a dis-
tance of ,,50, 000 krn from the
Moon), the landing, and the
first 5 minutes on the Moon' s
surface. The subsequent eight
intervals are related to operations
on !he Moon' s surface. Table 1
shows the accurate values of the
time intervals and the mean-
count rates recorded in these
intervals. The basic eirrors in
determining the count rato are
statistical.
Fig. 1. The mean-count rate ot "Luna-l'.
discharge count.er
The data in Table 1 iihow that the mean-count rate recorded on the
Moon' s surface was about 6316 of the count rate of the same counter in
free space. In other words, if only primary cosmic rays had been detected,
the counter on the Moon's surface would have counted not quite half as
much as during the flight in free space. The detected excessive radia:Uon
Card 2/8

ACC NR. AP6030010 Table 1.
Interval boundaries! Averaging intervai Mean-c:)unt I Nore
rate
131 Jan 1966 18 h 38 min 4U sec 10 h 12 min 30 sec 3.2291;).010 Duringtho
flight
1 Feb 1966 04 h 51 min 10 sec 10 h 54 min 20 sec 3.277to.010
15 h 45 min 30 sec
23 h 01 min 45 sec 017 h 16 min 15 sec 3.267to.011.
12 Feb 1966 16 h 29 min 00 sec 17 h 27 min 15 sec 3.278to.007,
3 Feb 1966 15 h 34 min 15 sec 23 h 05 min 15 sec 3.286tO.OO6
21 h 50 min 00 sec 06 h 15 min 45 sec 3.245tO.Ol2!Near the
Moon and
pn te M@Gn@
.4 Feb 1966 00 h 06 min 54 sec 02 h 16 m in 54 sec 2.065!0.016 !Un the Moon
06 h 35 min 04 sec 06 h 28 m i -. 10 sec 2.069t(1.010
17 h 02 min 00 sec 10 h 20 mi n 5() sec 2.074t(,.008
19 h 52 min 30 sec 0 " h 50 m i ri 30 st2c 2 . 0 7 7 (,. 0 14
5 Feb 1966 04 h 00 min 40 sec 08 h OH min 10 sec 2.058t(1.009,
19 h 01 min 40 sec 15 h () I ni i n 00 sec 2 . 0_5 5 1 (1. 006
20 h 37 min 30 s e c 01 11 35 m i n 50 sec 2.059t(l.020
22 h 42 min 20 sec 02 h 04 min 50 sec 2 059t(,.017,

The mean-coun t r ate during the flight is 3.272 tO .OO4
The mean-count r
Card 3/8 ate on the Moon is 2. 0600.004

ACC NR: AP603WIO
is 0.43 count/sec or @,26% of half the cosmic-ray intensity. This excessive
radiation may be due to the radioactivity of the Nloon Is surface and to the
secondary cosmic radiation produced by the primary cosmic rauiation in
the matter on the Moon' s surface region closest to the station (cosmic-ray
albedo).
Until now, no experimental data have been available on the radioactivity
of the Moon's surface. The "Luna- 9" measurements make it possible to
evaluate the radioactivity of the Moon' s surface in the landing area near the
Ocean of Storms. Assuming that the total detected additional radiation is due
to the radioactive gamma. radiation from the Moon' s surface, the radio-
activity of the Moon's surface may li, %20 times greater than that of the
Earth's surface (the count rate of "Luna-9" from the natural radioactivity
on Earth was 0.02 count/sec). However, the radioactivity on the Moon' s
surface has been evident"Ly overestimated, because the effect of multiplica-
tion of the primary cosmic radiation producing the cosmic-ray albedo
particle fluxes may expLain the major part or even all of the additi-nal
radiation detected. Using the data from an earlier Soviet paper, it can be
shown that the albedo particle flux is 20% of the total cosmic-ray flux or 401/0
of half the cosmic-ray flux- Additional considerations show that at least
in the region of the "Luna-9" landing, cosmic rays will be the main source
Card

L
ACC NR: Ap6o3ooio
of radiation hazarid and tnat the radioactivity on the surface of the Moon is
close to the radioactivity on the surface of the Earth.
It was shown during the flight of the second Soviet space probe in
September 1959 that at the distances greater than 1000 km from the Moon' s
surface, the intensity of the radiation trapped by a possible lunar rnagnetic
field does not exceed 10% of the cosmic-ray intensity. The "Luna-9" data
make it possible to evaluate the fluxes of the trapped radiation at digtance.-3
less than 1000 km from the Moon' s surface.
The mean-count rate just beforeand during the first minutes after the
landing was 3.25 1 0.012 count/sec (see Table 1). If this count rate is
corrected for the geometric shielding of the counter by the NToon during the
approach of the station to the Nloon and (luring the period of radiatinn de-
tection on the Moon's surface (this correction is about Ila), the resulting
count rate is 3.28 count/sec. This practicaliy coincides with previous
measurements. The time required for the "Luna-9" to cover the la:it 1000 km
to the Moon' s surface was ^- 2% of the time me asured in the aiven interval.
At the measuring accuracy mentioned above, an increase of 50% in the count
rate during this time interval would be noticeable.
-Card-5/8--

, -, 7; - - , _.
ACC NR: AP6030010
Thus the upper limit for the possible radiation flux penetrating the
Luna-9" jacket and trapped by the hypothetical magnetic field of the `Vloon at
the altitudes below 1000 km from the Moon' s surface is not more than half
the primary cosmic-radlation flux. The variation which would decrease the
intensity of cosmic rays might somewhat change the evaluation of the upper
limit of the hypothetical trapped radiation near the Moon, but the mai-i con-
clusions that the Moon has no radiation belts and consequently no marked
magnetic field remain Unchanged.
Fig. 2 shows the mean-count rAes in free space and on the Moon' s
surface. The intensity in the transition interval has been corrected for the
geometric shielding by the Moon.
It can be seen from Fig. 2 that the cosmic-ray intensity undergoes
slow gradual changes (solid curve) similar to those recorde-d during the flight
of "Luna-4. ",,/This makes it possible to assume that during the peri:)d of
the station's approach to the Moon, no appreciable variation in cosmic-ray
intensity occurred. Neither the available neutron-monitor data nor C-le
stratospheric data of A. N. Charakhchyan and T_N__CWr@hchyan (impub-
lished) revealed any considerable decrease in the cosmic-ray intensity.
Card

1, (,-1-C11-67
:_AOC _k @_._AP605_OCF1__O
couuc/aec count/Sec
4
Time of land ng
Reasurements durin Measurementa on
the Zoz
@O
0
0,
flight to t the Moon
@e _ I - I
1j S 5
Fig. 2. The count rates of the discharge counter during the "Luna-9" flight
in free space and on the Hoon's surface. The mean-count rate on the MoDn's
surface has been reduced to the mean-count rate during the flight, and the
scale has been changed in proportion to the mean-count rates during t@e
flight and on the Moon's surface.
The absolute flux of the cosmic-ray particles detected by "Luna- 9" was
-2 SeC-1. T he great error in the determination of the
equal to 5.35 10.5 CM
absolute fluxes is due to the 107o uncertainty in the operational dimer-s:7,ons
of the counter. Analogous measurements from "Luna- 7 ',',,-Ind "Luna-s"
stations performed on 4-6 October and 3-6 Dec`em_@er 1665 have shown t%e
particle fluxes to be 5.4 and 5A cm2 sec, respectively. The cosmic-ray
intensity in February 1966 decreased compared to December 1965. This
Card 7/8

ACC NR, AP6Q35o_i_c___--
ig. likely to be associated with the beginning of a new cycle of solar actJ-,,ity.
Thus the intensity maximum occurs during the period
December 1965-January 1966, and the lag in the cosmic-ray intensity
maximum behind the solar maximum detected for the protons of energies
higher than 30 Mev is about 1.5 years. This conclusion is also confirmied
by the data of the . "Zond- 3, " "Venus - 2," and "Venui3 - 3 " space probe G.
[FSB: v. 2, no. 101
SUB CODE: 22 SUBM DATE : 111-tay66 / ORIG RET: 003 / ani REF: 001
Card 818 Ev

.0DE_ -UR/0048/66/030/011/18'5/1817
ACC NRi AF7000527 SOURCE C
AUTHAOR: Lyublmov, FS
ORG: none
TITLE: .-.easuring the intensity of cosmic radiation by means of Zond-1, Zond-2, Zond-3,
Luna-5, and Luna-6 automatic space stations ZT-aper presented at the All-Union i-;eeting
on Physics of Cosmic Radiation held in IMoscow from 15 to 20 November 196-52'
SOURCE: AN SSSR. Izvestiya. Seriya fizicheskaya, V. 30, no. 11,
il,D66, 1815-1817
TOPIC Ti,GS: cosmic ray, cosmic ray intensity, cosmic ray measurement
automatic space station
i ABSTRACT: interplanetary automatic space stations of the "Zond" series
I
carried special Instrumentation for measuring cosmic ray emissions In i
C3
Interplanetary space and In the Earth's radiation belts. The Instru-
mentation consisted of scintillation and gas-discharge counters.
STS-5-type Geiger counters were mounted inside the spacecraft. Counters
of the SB'M-10 type were mounted inside Luna-5 and Luna-6. Results of
measurements obtained with the Geiger counters are presented. A com-
parison of daily mean values of emission Intensity measured by the
Interplanetary stations Indicates variations In cosmic ray Intensity
which are analogous to those recorded by the Luna-4 spacecraft. Maxi-
mum deviations from the mean values during measurements were +2% for
Cord

ACC NRt AP7000527
Zond-1, +4% for Zond-4, +5 for Zond-3, and +6% for Luna-6. '7hese
I - %
variations in cosmic ray intensity are relatZd to the presence! of spa-
tial magnetic inhomogeneities in near solar space and to variations in
the magnetic component of solar cosmic rays. A comparison of data on
cosmic ray intensity measured by Mars-1 and Luna-4 with data obtained
by Zond-1, Zond-2, Zond-3, Luna-5, and Luna-6 reveals a further in-
crease In Intensity. OrIg. art. has: 2 figures. I'WA-751
[JR1
SUB CODE: o4/
Card
SUBM DATE: none/ ORIG REF: oo4

LTUBIHOT, I., kand.sellskokhozyaystvennykh nauk
Hard of cows with high butterfat production. Nauka
v sallkhoz. 8 no.10:52 0 158.
(Dairy cattle)
pered. op.
(MIRA 11:11)

KALLISTOVY P.L.; ZETJKOV, D.A.; FHOKOFIYEV, A.F. PriniTrali uchastiye:
BOGDANOV, F.I-'.; BORWROV, V.I-*,.; BURYBLIN, A.V.; DROZDOV, M.D.;
YEROF-EirV, B.1*.;LCKISSA@-LOV, A.K.; YOGAL, I.D,; IZU-D-`-', I A.;
MIFIXI, R.Ye.; ROKHLITI, M.I.; SERGEYEV, F.V.;'T1Hk-V-" -A. D:;
FROWV, V.V.,- NUIATIONIA, G.F., red. izd-va; GORDIYENKO, Y 5.B. ,
tekhn. red.
[Instructions for applying the classification of resorves to
primary gold deposits] Instruktsiia po l.rimeneniiu klassifi-
katsii zapasov k korennym mestorozhdeniiar, zolota. Moskva,
Gos. nauchno-tekhn.izd-vo lit-i-j po Feol. i okhrane nedr, 1955.
46 p. (MBA 15:2)
1. Russia (1923- U.S.S.R.) Gosudarstvermaya korissiya po zapa-
sam po1eznykh 4.skopayemykh.
(Gold orea-Classification)

7,YUBIA7, IG010.
Trawlnrq put out to sea. V"
. pal 11 no.?1:1@-17 N '4f?.
(14IRA 12,--;)
(Travils ancl trawling)

SMIRNOV, G.; LYUBIMOV, I.
Put to use the potentialities of the Channel Dredging aza
MaintenAnce Fleet. Mor. flot 22 no.3:39--40 Mir 162.411RA 15:2j
1. Nachallnik otdela morskikh putey Glavporta (for Smirnov).
2. Otdel morskikh putey Glavporta (for Lvubimov').
(Dredging machinery).

. 11.
@LYUBJVIOV, I'*. A...
1,vubimov, 1. A.-JIVPV.RGBIITC PROMSSES IN THE POF
IIATION OF TFIP PETROPAVLOVSK immor
13ull acad. @.'SSII' Ser. gral, No. 4, 2.".1, (194'
(English summary 31).-L. shows that during bauxit
lotinatiou in this region the primary deposit was subjecte
to diage"etic and hyp@.rgcnctic mofifications. with the la
ter occurring to depths, of 150 to 2fX) ni. Up to 7% pyril
is present in tfic. deep zones. The irrrgular 3tructure of tl
underlying Silurian limestones ii due to FfsSO, arising froi
the pyrite.

0
0 41ho
40 4b
Oz
041-
0416.
Kv
L-YuBlil Ov I
10 1 It CPI
IL a
Lyubiscov. 1. A. OF DAUXITUS
Time" .1fetst.. 19 141 1-7,
I j1,41% , I W ,- 241.1110 Chemical mitudy%ell of nodb Ural
(VOKI *VrC tfCA@l StAtilitkUllY in M&V tO ObtAi--
jpvtirral pirtme ol thew depocitit. On this tia,.ix the
ijiv.kn, fm th- tituxite deltimits are: AIA 40 to W.
Fr,4), Li to 24. SM 3 to , TKII, 'i CnO 0.9 for the upper
Uy@r, and 1 9 to &6 fcw the Z.; h,.im x1co 0.6 to
0 9. C (not cuvintiat Cifbunatcs) 0.&% and S 1.1- 71W
combitied sum of At Fe, Si, Ti. " Afg. C. S, 0. Mid It is
VA)'-'. leavina lenthan I 'I for IS other elements determLard
in the anairses. The deviatkicis ftmn the meart, and
v4ru4titnts with It"ity depth of drilmits are given.
Ila-
ila
00
OG
00
06
Vatv& Wastfs all #a till 111C4,0411F 291114, It It 0 Q n t' It Is 4 1 A 0 5 1 1 1
41 0 0 0 41 0 41 0 0
i I, W-010MM, W - r

VINOGRADOV, S.S.; LYUBIMOV, I.A., redaktor; nMANOVA, G.F., redaktar;
KRYNOCHKI=@,'-kJ-.':- t@ icheskiv readaktor.
[Directions for applying the classification of resources to
dolomite and magnesite deposits] Instruktaiia po primeneniLu
klassifikataii zapasov k mostorozhdaniiam dolomitov i magne-
zitov. Moskva, Goa. nauchno.-tmkhn. izd-vo lit-ry po peologii
i okhrane nedr, 1955. 50 P. (MaA 9:,S)
I.Russia (1923- U.S.S.R.) Gosudarstrennaya komisslya po zapasam
poleznykh iskoyWoVkh.
(DO10mite) (Mapnesite)

&MMOV, V.I.; PROKOF'YEV, A.P.; BORZIRIOT, T.H.; DYUKOV, A.I.; ZHDANOV,
H.A.;_LYUBIH0j, I.A.; MIPMOV, T.Te.; PLOTNIECY, N.A.;
ANTROPOT, P.Ta., glavnyy red.; FEMMOVA, A.I., red.izd-va;
GUROYA. O.A., takhn.red.
[Estimation of res7rves of mineral deposits] Podschet zap3sov
mestorozMenit ppreznykh iskopaemykh. Pod red. V.I.Smirnova i
A.P.Prokofleva.@ Glav.red. P.IA..Antropov. Koskva. Goe.nauchno-
tekhn.izd-vo At-ry po geol. i okhrane nedr, 1960. 671 p.
(KIRA 14:1)
(Kines and mineral resources)

PosoLdye Dl--,,a Leu"-:ic,-,Ika -lr@juglw, 1-tell n,)-_o .- lo-,a @' rief ereM@.' j." -,.,Ie
'inc.-i ODe --ttor of P -red, er uy' Ljibi-mov. .-sxj
144 P.
.atalog uc! from Aus @,r:nc
Lle:rie,itari inforiviti-m .t.rtineat, t,
a. i nels IJLncri opurat-il"S .1 JV K I i L,4LI L IF 10 111, r: 0 IC . C -a! 11 5:11a
a@5 -,itjll as an,3 Pro,.:l.,c.' -'Il.
741.
.L)

TRUSOV, L.P. , inzh.; LYUB!:'CV, I. I. , inzh.
.9tandard plans of cylindrical reinforced concrete tanks for
petroleum products. Mont. i spets. rab. v stroi. 24 no.10:
30-31 162. (MEU. 15:10)
(Tanks-Standards)

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faurur) a high PrOtchi C