SCIENTIFIC ABSTRACT MUSTEL, E. R. - MUSTYATSA, V.

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• Collection: Scientific Abstracts
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• Document Release Date: March 14, 2001
• Sequence Number: 5
• Publication Date: December 31, 1967
• Content Type: SCIENTIFIC ABSTRACT

S/08ML/038/001/001/019
E032/E514
Results of a Statistical Stitd,
j ()I' Geomagnetic Disturbances for
Five Cycles of Solar Activit-Y
Table I
No'of Period Number of Itemarks
cycli investigated Plages Used
I if U f
14
15
16
1.1906-VI.1910 158 152
111.1919-1.1922 165 239 93
IX.1929-VIII, 118 195 71
1931
Most of the plages obtained
from the Kodaikanal and some
from the Meudon Observatories.
Active regions belonging to
Group II u weye largely taken
from o-S@ Observatory
data (Reg 81; some were taken
from the Nieudon data
Most plages from the Meudon
data, remainder from Kodai-
kanal and Mount Wilson data
Necessary information given
in Ref.9,
Cont,on next card

@' 93@ 20
S/033/61/038/001/003/019
E032/E514
Results of a Statistical Study of Geomagnetic Disturbances for
Five Cycles of Solar Activity
Table I cont,
No.of
cycl
1.7
18
Period
investigated
11.1940-
111-1943
V1.1951-
XI@1952
Number of
Plag;; Used
u
239 186 58
Remarks
Most plages taken from
Meudon data, remainder from
Kodaikanal and Mount Wilson
data.
75 111 63 Necessary information given
in Ref.9,
Total I.1906-XI.1952 755 883 285
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Results of a Statistical Study of Geomagnetic Disturbances for
Five Cycles of Solar Activity
In order to reduce the effect of flares (high activity) and
disturbances with anomalously long duration ZIT (lowest activity),
only those sections of the descending activity curves are considered
for which the relative sunspot number R is 15-20 R
Group II is further sub-divided into two sub-groups II and i1f,
which contain plages in the "unfavourable" and "favouragle"
hemispheres. The grouping is illustrated in Fig.1, The overall
results for the whole period are given in Figs, 6 and 7, where
Fig.6 refers to cycles Nos. 14, 15, 16 and 18 and Fig.7 to Nos. 14,
15, 16, 17 and 18. The general conclusion is that the only stable
formation on all the statistical curves is the maximum on the right
of CMP, The probability that the maximum on the right is accidental
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Results of a Statistical Study of Geomagnetic Disturbances for
Five Cycles of Solar Activity
is very small (this is said to be established in a paper in
a forthcoming issue of this journal). It is suggested that these
results confirm previous conclusions of the present author, namely,
that the active regions themselves are the sources of corpuscular
streams responsible for M-disturbancen (Refs. 1,2,6) and that
these streams are approximately radial (0. N. Mitropollskaya,
Ref.9). This conclusion is in agreement with recent radio and
polarization data (W. Christiansen and D. Mathewson, Ref.22;
W. Christiansen, A. Boischot, T. Kakinuma, H. Dodson-Prince,
Ref.23; G. Newkirk, Ref.24; J. Wild. K. Sheridan, A. Neylan,Ref.25),
It is argued that the negative correlation between active regions
and geomagnetic disturbances postulated by J. C, Pecker and
W. 0. Roberts (Ref.21) meets with serious difficulties. Among the
arguments put forward against this hypothesis are the following.
a) In distinction to the very stable maximum on the right, which
is present in all the statistical curves, the points to the left
of CMP are very irregular. b) Radio and polarization data (as
mentioned above) are in conflict with this hypothesis, c) Statistical
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Results of a Statistical Study of Geomagnetic Disturbances for
Five Cycles of Solar Activity
curves for plages with and without spots are practically identical
(0. N. Mitropol'skaya, Ref 4). d) Photographs taken during solar
eclipses show the presence of intense straight coronal rays at the
base of plages (Ye. Ya. Bugoslavskaya, Ref.30).
Acknowledgments are expressed to the personnel of the Meudon,
Kadaikanal and Mount Wilson Observatories for supplying the data
and to A. D. Grishin and S. Vlasov for assistance in the
numerical calculations. There are 8 figures, 2 tables and
32 references., 19 Soviet and 13 non-Soviet.
ASSOCIATION3 Astronomicheskiy sovet Akademiya nauk SSSR
(Astronomical Council, Academy of Sciences, USSR)
SUBMITTED2 August 20, 1960
Y

S/033/61/038/002/003/011
04 V/ E032/E414
,/ /a M1 / / ;, / )
AUTHORS: Mustell E.R, and Ayvazyan.. S.A.
TITLE@ Quantitative Analysis of Statistical Relations
Between Plages and M-Disturbances
PERIODICAL: Astronomicheskiv zhurnal ig6i Vol.,38, No.2,
pp@227-241
TEXT. In a previou8 paper (Ref.,I) the f@rst of the present
authors carried out a statlsti@al study of M-disturbances for
five cycles of solar activity It was concluded that, for plages
belonging to group 1, the only stable formation on all the
statistical curve5 con-sidered in Ref I is the right-hand maximum,
The aim of the present paper 18 to give a statistical analysis of
the results derived in Ref I using modern methods of the theory of
probability and mathematical statistics The principal aim is to
show that the right-hand maximum in the statistical curves plotted
for group I is not a random statistical formation but is real,
It is concluded that the geomagnetic field associated with "non
central" plages is time independent (on Lhe average) while the
mean strength M-disturbances in the case of "central" plages
varies with time in accordance with a definite and stable law.
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Quantitative Analysis E032/E414
This dependence can be approximately represented by two straight
lines with a maximum at t- + 6d, A typit-al zurve of this type is
shown in Fig.3,, This figure refers to group 1@ @_ircles are
experimental and the dashed 1-ur-vt;; 1.4 the theoretical fit, The
probability that the foim of the cur-/e is a!s shown by the dashed
curve in Fig,3 rather than random variatic;n about a mean is
3.1 X 109@ Varian--e analysis, X 2 test, regression analysis,
method of least squares etc, are used to confirm, and give a
statistical basis for ' the conclusions drawn in Ref.l,, It is now
definitely established that the passage of plages across the
apparent centre of the solar disc is &:.companied by geomagnetic
disturbances, Acknowledgments are made to corresponding member
AS USSR N.V.Smirnov for advice and consultations and to
A.S.Dvoryashin for his assistance with data, There are
5 figures, 8 tables and 9 references. 7 Soviet and 2 non-Soviet.
ASSOCIATIONS: Astronomicheskly sovet AN SSSR
(Astronomical Council AS USSR)
Matematicheskly institut AN SSSR im, V,A,Steklova
(Mathematl,--s Institute AS USSR imeni V,A,Steklov)
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MUSTELI . EA,,
Corpuscular stream az* the solar corona. above active regions*
Astrono-sk-r- 38 no*3085-401 W-Je 161* (MIHA l4s6)
1. Astronouioheakiy sovet AN &SSR.
(S=)

S/035/62/000/007/024/083
AGO1/A1O1
AUTHORS: Mustell E R., Kopylov, 1. M., Galkin, L. S., Kumaygorodskaya, R.N.,
TITLE: Spectrophotometric study of Nova Herculis 1960.
PERIODICAL: Referativnyy zhurnal, Astronomiya i Geodeziya, no. 7, 1962, 31,
abstract 7A236 ("lzv. Krymsk. astrofiz. observ.", 1961, v. 26,
181 - 216; English summary)
TEXT. About 120 spectrograms of Nova Herculis and t@Aql taken as a standard
were taken in March - April 1960 with the 122-cm reflector of the Crimean
Astrophysical Observatory, mainly with a quartz spectrograph with dispersion of
155 A/mm at H7. The following quantities were determined: equivalent widths
W A- and values of L"j,\ (km/sec) f or emission hydrogen lines H@419, as well as central.
intensities 10 with respect to continuous spectrum for all iaentified emission
lines in the spectrum of N Her. Changes of these characteristics of emission
lines in the course of time were generally analyzed. The average speed of enve-
lope expansion was estimated (1,85o kr4/sec) from the width of hydrogen lines.
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Spectrophotometric study of Nova Herculis 1960. 1. AOOI/A1OI
Approximate brightness and date of maximum luminosity of N Her were determined
from spectral changes observed in this Nova: mmax - 2T50tOT17 (probable error);
March 1-k2d5 (probable error). The absolute magnitude of the Nova in maximum waz
determined (Mv - -10TO), as well as distance to the star (R 1,250 Pc) and total
interstellar absorption in visual light at star distance (Av 2TO). By com-
paring with @ Aql relative energy distribution was obtained for each night in
continuous spectrum of N Her within the wavelength range AA3,512 - 5,050. Balmer
decrement was calculated from lines HA-Hq. There are 12 references.
From authors' summary
[Abstracter's note: Complete translation]
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33422
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3--;-L130 L! 14
A I; MOR Nfits t p I E , it,
F I It. )m the "cone (it ivoioant. e" hvvo t he-; i in t tit- nrot) I em o i
I. he orl q i n of' rorim -;cu I rit, -A t t* e in tit -;
P tL 111 oD I C,% I, Xs t ronomi chosk i v /tit I r n a I @ L4 tit) 4 '7
FFX I : r 11 e a n t tio r- c (im ri a r t it (- r r) n v (i i it vo i (1a it c f@ h no ti(-@- i s
I ite I I ; C. W A I len , '-Ion t It I I , tlov A I ron oin . St, c 1011 1 -,,
t 44'1 If (- C 2 , J C PecRor, (I. Hilbert-, J(,)tll-ti of (wol,flvs ! z p --, '
t),j , i 11-155) and t tie act I v e- r(,-4Z I o n tiv (m fle@ I s ativ a ric vit b v t he
tir e sen t ill t hor i n t) r ev, oil - i)a yiers ( fie U, 1 As I ron - / h - . 36, 16 1)
I ()b I I R e 1', 4 Ib I d, 28, 140 1 ) , A c co rd i ng to the for-mer
it c t i v e r eg i ons t. hecuse I % p -4 a r f- n (i t a @ oil rc e o I co r Pit s c u I it r s t r vam s,
*-it c h it c t i v v r eg i u n in e re I v de I I vc I @ I o on" @ I de t lie ,ir e 1) v r-, I I
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themse I v es , whi I t, I fie L maxi itimn 1 4 dilt- t 1, 1 11 o 1';i c t t ho t t lie filvist)
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33422
On tit(- avotd.--ince"
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days.For each of these ;-rtmos IIt+, stitierl'osed riorh CqlT-v(- i s
r,- p I o t t ed , %ccord i fig to t ht- iic Iiv e - r- --g i )if h , im I he- I - on I N, t tie
- I zli T ha nd Illei x I milln , holt I (I r v I cl I if III M) I I t I I in I it t h I S a fla I vs i
wh i I f- v tie Ie Y-t ma x itmom -;h(m I it sit I Iii mia rd q t tie I e Vt a s A L'
1 11 ( I' (1 .1; p a it d t h e r f @ q it o I i I (I h p , i IIf if, a r r v IIf t i f) n bet wo-en t It e
nos i t i r. it r) f t h i s mit x i mum a tit] 4L Oimt,t I c -i I ca I c u I a t i o ns
carri ell out for ab-I 1 700 1, 1 ;1 zf- Q Ito %v -hotol II i.-itt he-Ap pred I c I i ntis
0 1 1 ne ol. t i ve-regi on hvno t ht.s I @i I I p! n I @-l i I c o if I IF-Irl ed r It n
Ina x i mitm do es s 11 t. Ct t o t h t- I f- I I ;md i tir rf- I a f ioti hefi,-et-n 1- it f-
nosi tion of- the maximum ;,fill A I. I nt.,, I tie , ,Tic itisi-on
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and it re i n con 17 1 i c t xvi t If the cone o I , %, (... I -i it c e It,. r- t h P @; I s ri
partictilArt for Adl- ditVS ttli-I 4- Ls rt(i im;ixtmom ;it the Lkfi' I i tie
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On the "cone of avoidafice" S/011/62/0'51)/001/004/011
1,'032/Fr, I If
(A t = 0) a I thoitzh t h i s woti I d be P yn-, # , I ,n t lie rnnp n f
avoidance theorv, Fi na I I NI, t h c ef f ec t of varia t ions in the
,geomaynetic field on the simerposeo @tjivvs Is
[t tiiriis oxit that tho left-hand nar-t of* thf, inti-irral corve ts
comnoged of isolated and relativelv hicrh L. rri.-INima corresT)onditig
to differentA L However, ouring, to intt-rference nhenompria
disciissed in Rof cIt the left-hand sirle (it' the ititegral ctirve ,
im,livding the L maximsim, i-s invich Inwet- than the R maximom, Th i
I @ @,) i d to indicate once r"ore that t tie oo I v stable Format ion on
t h v sti i)ernosed epoc h c u rves wh i c h has a I o Ci ni t f, nhys i ca I s i KII I
t i cane p i s the r i t@h r@ ma x i mitm , The ma i n rea son fo r t be rethic t i ori
i n t h e t'i eld amp I i t ii de oti t. lie i n t egra I cu t-v e o f th e -m net-nos od
e poch tire t hod i s the m1i ttia I sli per-po -; i t i oo o V M- d i s t lirbavic es .
rhere a re I f igii ir-es a rid 9 re feren c PQ . 9 io vi e t - b I oc a rid 4 non -
Soviet-bloc. Th e ng I i sh - I a ngionge references r-pad as fol low.;
Refs. I anti 2 qiioted in text ; 1?(-1*. 8: F.Wat-d arid R@ Shanit-o, Jmir-n.
of Geoph.Res., 66, 7-)9, 1901, Ref 7: G Newki rk, AstrophYs.Joiirn,
i3-)j 983, ig6i.
ASSOCIATION* Astronomicheqkiv sovet Akademi l- nauk SSSR
(As t i-onomi ca I Colinc i I ot' the Acadenty of Scienc(-s
s U 8 m i,rr E D September 10, 19bl S It
Car(] V3

-' @ I @:-f i L4
'@10 - 1039/002/001/014
e' 01
AUTHOR: Mustell, E.R.
TITLE: Novae as a nossible source of c,i,;mi, roys
PZRIODICAL: Astronom h- kiv zhurna I , v. 39, no.2, l962, 185-1
TEXT: The author . . ..' a criticil discussion of the mechanismg
which may be respunsible for the replacement of the pre-maximum
spectrum of a nova by the principal spectrum. This
replacement is a universal result for all novae and suggests
the presence of certain forces which accelerate zases ejected
from the novae im, ..' itely after the light maximum. The review
given in a previoo.- -1per (Izv. Krymsk. astrofiz. observ., v.4, 23,
1949) is critic-11 reconsidered. Tho following- acceleration
mechanisms are (iLscussed: a) shock %v.,vP.. h) acceleration of
the detached envelope by gas condensations -$nd c) light pressure.
In addition, a critical discussion i.. giver if the hypothesis
according to which the pre-maximum and principiil spectra are due
to.the continuous outflow of gases whose intensity and velocity
undergo a change near the light maximum. All existing
spectroscopic and other obserrvations are shown to indicate that
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Novae as a possible source ... 9032/E414
none of these mechanisms is satisfactory. It is concluded
that cosmic-ray pressure is mainly responsible for the
acceleration of the envelope. It is argued ttiat the inter-mediate
ficavity" which appears immediately after the 1-kght maximum between
the envelope and the star is filled by cosmic rays. The
quantitative onsequences of this cosmic-ray hypothesis are worked
out and a formula is derived giving the total cosmic-ray energy
f Lx entering the inner pa ts of the separating envelope.
TiJ3 flux is ENR - 5 x IOU erg/sec (on the average, for a
typical nova). The losses experienced. by cost,iic rays are
discussed. It is estimated that the fraction of cosmic rayc;
leaving the envelope for interplanetary space is approximately 0.1.
The paper is concluded with a discussion of the interaction of
cosmin rays with gases in the detached envelope in the presence
of frozen-in magnetic fields. It is estimated that the mean
energy of all Ges"Ite rays lunl@ in
,otreduceA durins the nova oxrjlcplj
0 There are 2 figures.
the Galaxy in about 4 x erg/sec.
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Novae as a possible source ... E032/E414
ASSOCIATION: Astronomicheskiy sovet Akademii nauk SSS:?
(Astronomical Council,Academy of Sciences US510
SUBMITTED: October 1, 1961
i
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AUT.'!()IrZ: @Iustel', E.R.
31V'
3/033/62/039/003/002/010
E032/Ell4
On the spatial structure of the solar corona. Part I.
LIL:,;,iujICAL: Astronoir:icheskiy zhurnal, V.39, no-3, 1962, 418-1127
CE X'r This paper is concerned uith general problems
associated with the structure of the solar corona, with particular
reCerence to corDuscular streams. ln the first part the author
argues that the presence of relatively intense middle-latitude
remions with I-1-rays (streamers) and also much less developed
eqnatorial and polar regions of the so-called intermediate corona,
reflects the large-scale characteristics of the sun (general
magnetic field, surface distribution, rotational characteristics
and so on). On this approach the role of active regions is of
s6condary importance and the average density of the corona in the
equatorial belt (between active regions) is less than the average
density in the belt of =-rays. This is responsible for the
lower brightness of the corona in the equatorial belt. One of
the strongest arguments in favour of this hypothesis is that,
contrary to the alternative cone-of-avoidance hypothesis, the
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solar corona is denser over active regions than over Qther ray
structures. Next, a discussion is given of the main geometrical
properties of 11-rays. Particular attention is paid to the size
of these rays and it is argued that according to the available
evidence the total length of these rays is of the order of
30-50 solar radii. Even if the rays do reach the earth's orbit
they must be very weak, and in any case they cannot be the source
of M-disturbances. It is argued further that there is little
point in comparing coronal rays obtained from eclipse photographs
with geomagnetic disturbances, or in deducing the corpuscular
delay time from such comparisons. In the final part of this paper
the author discur-ses a recent article by ITA. Waldmeir (Zeitschrift
fuer Astrophysik, V-53, 1961, 198) who investigated an eruptive
prominence and came to the conclusion that the motion of the
latter occurred along a I-I-ray and was determined by the "solar
wind". Fie concluded that rl-rays are in faet stationary gas
streams. It is suggested that the coincidence of the trajectory
of the prominence with the general contour of the corresponding
coronal 11-ray was fortuitous so that Waldmeir's conclusion
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cannot be accepted.
ASSOCIAI'10N: Astrono;-.,icheslciy sovet AN SSSR
(Astronomical Council, AS USSR).
SU B@Nl rT ED: December 1, 1961.
x
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3, SVD E032/E514
AUTHOR: Mustell, E.R.
TITLE; On the spatial structure of the solar corona. Part II
PERIODICAL: Astronomicheskiy zhurnal, v-39, no.4, 1962, 61g-631
TEXT: This paper is a continuation of previous work
(Astronom.zh., 39, 418, 1962). It is concerned with the
following problems. the structure of coronal rays above active
regions (AR-rays), comparison of P-rays, i.e. rays above quiet
prominences-filaments, with AR-rays, and the comparison of
optical eclipse observations with radio-astronomical and
polarimetric observations of the corona. The gas densities in
AR-rays are discussed again and it is shown that these rays are
the densest coronal formations. This has been confirmed up to
distances A R 2R . The form of the AR-rays is discussed.
It is shown that wiThin the range nR,< 2R the eclipse
observations of Ye. Ya. Bugoslavskaya @Tr.oGos. astron. in-ta im.
P. K. Shternberga, 19, 1950) are in complete agreement with
G. Newkirk's polarimetric data (Astrophys. J., 133, 983, 1961).
The geometrical properties of AR-rays at large distances from the
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sun are discussed and it is shown that there is considerable
evidence for the fact that these rays extend over very large
distances, reaching the earth's orbit 'and are approximately radial.
The origiii of the departure of these rays from the strictly radial
direction is discussed and it is noted that these departures are
largest for the rising branch of the solar activity curve and
smallest for the descending branch. It is also noted that there
is now considerable published evidence for the fine structure of
AR-rays at large distances from the sun. A comparison is
m,adle betwPen -he geometric and physical properties of P-rays and
AR-rays.The resuLts are given in a detailed table in which the
properties of the two types of rays are compared and contrasted in
detail. Inspection of this table shows that the two types of rays
are fundamentally different. Fig.2 is a schematic drawing
illustrating the contrdsting properties of AR- and P-rays. The
left-hand side of the drawing (which is not drawn to seale)
bli" Av#eA#p tatitude of' maximum frequency of
occurrence of active regions, while the right-hand side corresponds
to the average latitude of the maximum frequency of occurrence of
-.Iuiet filaments, i.e. P-rays. The right-hand side shows the
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effect of the rotation of the sun, the narrowing of P-rays at the
erids and the relatively short length of these rays. The left-hand
side shows that AR-rays consist of isolated "tubes" leaving the
active regions ABC etc. The final section is concerned with
coronal rays in the active region belt but not in the regions
themselves. It is shown that these rays should be similar to
AR-rays but should have a lower gas density so that they cannot
give rise to appreciable geomagnetic disturbances. The data
reported by H. S. Bridge et al. (Publ. of 1961 Kyoto Conference
on cosmic rays and the earth storm) are briefly discussed in the
light of these results. There are 2 figures and 1 table.
ASSOCIATION. Astronomicheskiy sovet Akademii nauk SSSR
(Astronomical Couniril, AS USSR)
SUBMITTED: December 15, 1961
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AUT14OR:
TITLL: Longitudinal distribution of active solar region.-%
;And the problem of corpuscular disturbances
PERIODIC%!,: Astronomicheskiy zhurnal, v.39, no.5, 1962, 813-832
TEXT: 'rhis is a continuation of previous work by this author
et at G%,-,tron. zh., v.36, 1959, 215; v-38, 1,961, 28; v.38, 1961,
389; v-35, 1958, 194; v.36, 1959, 5;' V-39, 1962, 41; v-39, 1962,
big; v.38, ig6i, 227; Izv. Krymsk. astrofiz. observ., v.27, 1962,
167; Dokl. AN SSSR, v.42, 1944, 117)- In the present paper,
the influence of the longitudinal distribution of active regions
(plages) on the characteristics of the SEM (supe'rimposed epoch
method) curves is investigated. The-observational material
includes plages which passed through the visible centre of thg
solar disc during CMP or very near to it. The data were
.obtained from an examination of several spectroheliograms
covering the interval 1907 -1952. The entire interval is divided
into 12-periods and the results of the application of the SEM are
shown in Figs. 1 and 2. It is apparent from these curves that
Clard -1 1A -3 .1

S/033/62/039/005/002/011
Longitudinal distribution ... E032/E314
their most stable characteristic is the main maximum P , which is
always preceded by the minimum M i n Frequently, there are
further maxima R' and L . The form of tile SEM curves at
6t = -121 and +156 is r-ougfily the same (effect of tile 27-day
recurrence). A detailed statistical analysis is made of these
distributions, in whi.ch histograms are obtained giving the
distribution of the number of equal distances between neighbouring
plages as a function of these distances for each of the above
12 periods. It was found that all the histograms had clearly
defined maxima. This analysis is followed by a general
explanation of' the presence of the R, R' and L maxima and of
the minima Min on the SEM curves which is then used to analyse
each of the curves separately. The main conclusion is, as before
(the present author - Astron. zh., V.39, 1962, 41), that the only
stable maximum on tile SEIM curves is the R maximum and that all
the remaining characteristics of these curves are due to the
longitudinal distribution of active regions. The final section
of the paper is concerned with a critique of Saemundsson's paper
(Monthly Notices Poy. Astron. Soc., v.123, 1962, 299) which is
Card 2/41")

S/033/62/039/005/002/011-
Longitudinal distribution ... E032/E314
also concerned with general statistical aspects of ' the origin of
1-1-disturbances. Sacmundsson has reported some d
oubt as to the
present author's conclusion that central plages are responsible
for 1%i-disturbances. It is now argued that Saemuridsson's analysis
suffers from the following shortcomings: 1) the analysis was
based on inadequate observational inaterial, 2) the model used was
not directly related to the previous analyses of the present
author (cf. references at the beginning of this abstract) and
3) Fig.13 of Saemundsson's paper is based on plages with very
different latitudes and hence does not materially contribute to
the problem at hand. For these and other reasons the author
considers that Saemundsson's conclusions are inc4orrect. There
are 15 figures and 2 tables.
ASSOtIATION: Astronomicheskiy sovet Akademii nauk SSSR
(Astronomical Council of the AS USSR)
SUBMITTED: December 15, 1961
Card 3/,$ 3 .1

MUSTELI -, E.
*Mars-10 is in flight. Av. i kosm. 45 no-11:8-10 '62.
(MIRA 15:1-1)
1. Chlen-korrespondent AN SSSR.
(Space flight)

GURZADYAN, Grigor Ararnovic-h-, krBARTSUPEAN, V.A., red.; MIUSTEL"L E.E.,
red.; SEMM , A.B., red.; SOBOI-EV, V,V., red.; KULIKQVy
ITO
G.S..' red.; BRUD'i , K,F,, tekhn. red.
[Planetary nebulae]Planetarnye tumannosti. Moskwj, Gos.izd-.vo
fiziko-matem.lit,ry, 1962. 384 p. (MIRA 15:9)
(Nebulae)

-MATBL I I -
Analysis of the chemical composition of enve-lopes of novae.
Astron.z,hur, 40 no.6zlOO7-1012 N-D 163. NIRA 16: 11)
1. Astronomi:iheskiy sovet, A@.' ISSP.

KAPLAN, Samuil Aronovich; PIKELINER, Solomon Borisovich;
A14BARTSUMYAN, V.A., red.; MUSTELI E R red.; SEVERNYY,
S red
A.B. red.; SOBOLEV,
AKSELIROD, I.Sh., tekhn. red.
(Interstellar medium] Mezhzvezdnaia sreda. Moskva, Fiz-
matgiz, 1963. 531 P. (MIRA 17:2)

MUSTELI,E.R.; BOYARCHUK, A.A.; WTASH, T.M.
Energy distribution in the continuum of M Aquilae 1918 and RS
Ophiuchi. Izv. Krym. astrofiz. obser. 30:19-24 163.
OGRA 17:1)

L 18935-63 BDS aW
ACCMION NRs AnOO3326 5/=6/63/000/006/0017/0024
AUTHORs -.Vustell, Ee g,.I_C'orTesponding Member of the Academy of Sciences of theSSSR
TITLEs Solar corpuscle'o@ tile interplanetary medium
SOMORt Priroda, no. 6,, 1963, 17-24
MPIG'TAOSt "solar windp" comet tail, "frozen-irP magnetic field,, geomagnetia
storm,, interplanetary spaceI corpuscle stream
ABSTRACTs The earth actually 4es within the outer part of the vlar corona. V. A.
_Kratt and associates at W14iave shovm that the chro )spher* is a complex, un-
homogeneous formation consisting of separate fibers and clusters with different
temperatures. The gaseous component of the interplanetary medium is made up almost
entirely of corpusoular radiation from the sun. Even when there are no active
areas (sun spote),, the sun is constantly emitting a stream of corpuscles. Hence
the corona. cannot be regarded like the earth's atmosphere as a sort of hydrostatic
formation* The latest theoretical work and rocket research have shown that it is a
dynazzdc,, constantly expanding medium, in each point of which there are fields of
corpuscles moving from the sun with different speeds, densities., etc. This has been
called the "solar windv" though it differs radically from terrestrial winds in
Card 1/3

L 18935-63
ACMSION NRt AP3003326
temperature,, density$ speed and many other characteristics., The latest research
'has shown that the sources of corona heat are so great that it cannot be in equilib-
ftum. The article gives the speed and density data furashed by Soviet and American
(Mariner 33) rocketat 450 km/sec,, 10 sup 8 cm sup -2 see sup -lp average density
,,About 2*5 particles per 1 cu emo No S. Robroy in the Astro-Council of the AS USSR
1concluded that the intensity of the disturbances on the @po @-capsFRardly depends
I at all on solar activIty,, i.e. the outflow of gases from the sun is stable. L. Bir-
_'man has advanced the hypothesis that the gases emitted from the nucleus of a comet
!are driven away by the solar windj, light alone being insufficient to turn iti il
- away from the am,, an thought heretofore. But the density of the gases is too low
:for this t one muAt also take into account magnetic fields "frozen" into the corpus-
cular streams., In Interplanetary space we have to do both with individual condensa-
tions moving almost strictly radially and with these corona rays assuming a curved
form due to the sunts rotation* A22 rocket observations, Soviet and American indi-
cate that areas completely free of a magnetic field are very rare in interplanetary
space. It may measure from a few gawtas oVtiU days to 20 or more during geomag-
netio disturbances* 7he xeomagnetic stormd@, recurring every V days (sun rotation
time) are believed to be due to the periodic sweep of a stream of corpuscles from a.
fixed source somewhere on the sun* It ;nay be considered that about 4-5 days after
a calcium floccule (active area) passes through -l'.16 visible center of the solar disc
Card 2/3

L 18935-63
AMMSSION MRj AP3003326
1 0
the earth enters a stream of corpuscles and the disturbance begins. There is every
reason to believe that the elasticity of these rays is due to the magnetic field
"frozen into them." The author's preliminary calculations show that such elasticity
requires fields of 1-10 games, precisely the order of magnitude of the fields mea-
sin-ed in interplanetary space* The density of the corona, over the active areas is
about 10 times greater than over the rest of the sun's surfacee In any case inter-
planetary space in not amorphow,, but has a structure; indeed# its main features may
be sketched in fair detail,, with a system of curved elastic coronal, rays playing one
of the main roles* But much work remains to be done to convert this into a precise
.model* Orige has 3 graphs., 4 diagrams and 1 photo.
ASSOCIATIONs none
SIUBMITTEDs 00 DATE ACQt 26JV163 EMLs 00
SUB CCDZs AS NO REF SM 000 arms 000

MUSTELI, E.R.
-'-, 61iim on the Physics of Chromospheric Flares. Vest. AN SSSR
34 no.3tll9-120 Mr 164. (MIRA 17 14)
1. Chlen-korrespondent AN SSSR.

MARCHUK, A.A.; MUSTELI, E.R.
Line spectrum of the "old" Nova Aquilae 1912 (V 603 Aql).
Astron. zhur. 41 no.3:587-589 MY-Je 164. (MIRA 17:6)
1. Krymskaya astrofizicheskaya observatoriya All SSSR i
Astronomicheskiy sovet AN SESR.

MUSTELty E.R.
Solar ,!rrullmo ;@Tj 1 n-zi-@jr. 41
no.5:77'?-8CXj S-ri 164.
1. Astronoinicheskly soveL 91 SL@,R.

MUSTELIS E.R.; MOGILEV-ShlY, E.I.
Solnr activity and the gecele,::trlc c-mp-e/ of
biul. no.14:92-015 164. (Ml`@A 18:4)

ia r
tp_ Cl y
C njr-

t:A!31-0@66, aW
AR60284LIS SOURCE CODE: UR/0269/66/000/005/0055/0055
-7
AUTHOR: Mustel' , E. R. Bonelis, 1. V. ; Kq@@s4ISLin,_Y. V.
TITLE- The effect of cosmic rays on the lowest layer of the Earth' s atmosphere
SOURCE: Ref. zh. Astronomiya, Abs. 5. 51. 429
REF SOURCE: Astron. tsirkulyar, no. 333, iyulya 10, 1965, 1-6
TOPIC TAGS: cosmic ray, atmospheric pressure, chromospheric flare, solar
flare
ABSTRACT: According to Soviet and Western Europe weather bureaus, the
earth' s atmospheric pressure increases on the 6th day after an active area
passes through the center of the solar disk (an average of 13, 878 active areas
during the 1907-1952 period). This fact correlates with an increase in greorna@ne-
tic activity. After chromospheric flares, the atmospheric pressure on the Sull
increases sychronously with an increase of geornagnetic activity (on the 4th (Jay
after a flare). Thus, the effect of solar corpuscular streams causes an increase
Card 112 UDC: 523. 75:523. 165+ 525. 24

L -47310-66
ACC NR: AR6028405
in atmospheric pressure. At the same time, a decrease in atmospheric pressure
occurs in the area of geomagnetic polar caps immediately following flares. The
-istic
authors have associated this phenomenon with the activity of subrelativ
proton streams. Orig. art. has: 9 reference items. G,' Ivanov@Kholodnyy.
[FMI
[Translation of abstract)
SUB CODE: 03
2/2

I F .-, . ;F" -.
IT S TE 1.
Az,alpji-,l or
Oumntivaliv- afialy4in
L ri zhtness. As tron. 7 lv-ir vo.
An t

cular__streams.-from@_-tlae-sm
7-1
_'@@Soullwxiz tronomicheskiy zhurbal v, 42., no* -1
TOPIC -:-TA -so --ra ti6@
-I'm dia -4olar_ activity Padio' abso l6n, c6smic ra3
lpt
r
wave
space,;pro e

- - @ :.- - @ - -, - , - - -j - .1,11@ I , - @ @ 5 ,- " -@@ -L @@- @@ @-_, :-- , , ,. -, --- -, 1. - - . -:1 , .
. , . .@ @,- . i -: . . @ - -- : -.1 . 1; .1 . . . - I -- ---

SOIRCEr:., Astronomicheekly ghurnal, v. 42, no. 6, 1965, 1232-1249
iIA46rological,pheno non,, proton stream, corpuscu
JOPICIAGS: me
flare
ABSTRACV@ Quast-stationary corpijacular fluxes emanating from active regions during
6dbf l45l_to-i95j_aii'Laiii3l_yzed. Chrdmospheric flares recorded at several
the.-pert d
-Atct Ic. stat Al plotted diagramatLcally.
n cates @_tfiai 'tW-:co-rpuscular streams produce a pressure
at
A
increase.. subrelativistic: proton streami -.f ion. chrosospheric flares
duC6 ViC4
pro sure decreases at t polar. caps It to noted-that the amplitude
',decreas0@::_of,.atmD5pWrIc' disturbances- with decreasl@&:. gnetic latitude can be
geo"
ation. This'assumption Is borne out by
a source-buaddIt cas atmospheric, circul
-'analysts: of-. thko, spr c detailed discussion of all
ht I f are
ViC. _523.145
CWd 1/2

0
13 figures
Wj I
ATO PRESS:
4m

ACC NRt AR6028766 SOURCE CODE: UR/0269/66/000/006/0062/0062
AUTHOR: Mustell, E. R.; Yegor-ova, N. B.
TITLE: Comparison of geomagnetic excitations with phenomena on the sun
SOURCE: Ref. zh. Astronomiya, Abs. 6.51.479
REF SOURCE: Sb. Solnechn. aktivnost'. No. 2. M., Nauka, 1965, 5-52
TOPIC TAGS: solar phenomenon, solar activity, solar flare , geomagnetic measurement
TRANSLATION: Comparative studies of recurrent geomagnetic excitations and flocculi pas-!
!sing through the center of the solar disc, and of sporadic geomagnetic excitations with
chromospheric flares performed previously (See RM Astr., 1963, 11.51.385) during the
iperiod I July 1957-31 December 1958 were continued to 31 December 1960. Two tables
with data on the chromospheric flares and the resulting sporadic geomagnetic excita-
tions for the periods 1924-1957 and 1957-1960 are included. In addition, there are 27
charts for 1959-1960 comparing the time of the passage of flocculi in the innediate vi-
,cinity of the center of the disc through the central meridian with moments of bursts of
.type IV radio frequency radiation, and with the beginning of geomagnetic excitations.
':The charts show a separation of 14 recurrent geomagnetic excitations, and their corre-
,sponding stable active areas. The following conclusions were obtained from an analysis.
@of the tables: 1) the flares causing gemagnetic excitations are homogeneously distri-
UDC: 523.75:525.24
Card _1/2

ACC Nk. AR602876j---
buted over the solar disc; consequently, they emit particles in all directions. How-
ever, the very strong sporadic geomagnetic excitations are caused by flares near the
central meridian; 2) the mean time of motion of corpuscular streams toward the earth is
d
:2 ; this time does not depend on the heliographic latitude of the flare. For more power,-
Iful flares, this time is somewhat shorter; 3) bursts of type IV radio frequency radia-
,tion accompanied 55% of the flares which caused geomagnetic excitations; and 4) the
,presence of a flare is not a sufficient condition for the occurrence of a geomagnetic
:excitation. 15 refetvnces. M. Gnevyshev.
SUB CODE: 03
Car

L 023139-67 bUT ( 1 CVd
ACC N" AR6029442 [N) SOURCE CODE: UR/0169/66/0001005/AO47/AO47
AUTHOR- Mu stel E. R Yegorova, N. B.
TITLE: A comparison of geomagnetic disturbances with solax phenomgna
SOURCE: Ref, zh. Geofizika, Abs. 5A281
REF SOURCE: Sb. Solnechn. aktivnost'. No. 2. M., Nauka, 1965, 5-52
TOPIC TAGS: geomagnetic disturbance, solar phenomenon, chromospheric flare,
flocculation, solar flare
ABSTRACT: A comparison (See. IlZhG fiz, 1963, 3A244) made previously for the
Iperiod from July 1, 1957 to December 3 !, 1958, was continued until December 3 1,
1960, between recurrent geomagnetic dii;turbances with floccula passing through
the apparent center of the solar disk, and sporadic geomagnetic disturbances with
chromospheric flares. Tables were given with data on chromospheric flares and
the resulting sporadic geomagnetic diStLrbances during 1924-1957 and 1957-1960.
Fou rteen recurrent geomagnetic disturbances and their corresponding stable active
regions were delineated on 27 maps for 1959-1960. These maps compared the time
Card 1/ 2 UDC: 550. 385:523. 7

L 02339-67
ACC NRs AR6029442
when the floccula. passed through the center meridian at the moment when they are
in an earthbound direction with the times of radio emission type-IV surges and the
beginning of the geomagnetic disturbances. The following conclusions were reached:
1) Flares, causing geomagnetic disturbances, are uniformly distributed over the
Solar disk, which implies that particles are thrown from it in all directions. How-
ever, the very severe sporadic geomagnetic disturbances are caused by flares, near,
the central merL'dian. 2) The average time of the path of corpuscular currents to
two days and does not depend on the heliographic lattitude of the flare. This time to
much shorter for more powerful flares, if another disturbance preceded the given
geomagnetic disturbance. 3) 55% of the flares which caused geomagnetic distur-
bances were accompanied by IV-type radio emission flares. 4) The presence of a
flare to not the only condition necessary for causing a geomagnetic disturbance.
Orig. art. has: 15 reference Items. M. Gnevysheva. [Translation of abstract].
SUB CODE: 03/
2/2

ACC NR: AP6032664 SOURCE CODE: UR/0203/66/006/005/0815/0821
.AUTHOR: Mustel', E. R.; Haysuradze. P. A.
@ORG: Astronomic Council, AN SSSR (Astronomicheskiy sovet AN SSSR);
:Institute of Terrestrial 211agnetism, Ionosphere, and Propagation of Radio;
Waves, AN SSSR (Institut Zemnogo magnetizma, ionoofery i resprostraneniya
radiovoln AN SSSR)
!TITLE: Radial dimensions of corpuscular stream from a chromospheric
I
,flare and thetime during which the earth wa-a located in the stream
!SOURCE: Geomagnetizm i aeronomiya, v.*6', no. 5, 1966, 815-821
TOPIC TAGS; chromospheric flare, magnetic perturbation, corpuscular
stream, sudden magnetic storm, radiation belt, magnetosphere, horizontal.
component J S-0 4.,ge 0'x4 Ae. %5o4.1?,q clHeol7@,YPNE!,eFS, %-,FoLg P- Cott? PvS cu4,,qe
'ABSTRACT: Intense chromospheric flares last less than 2. hr, but
sporadic magnetic perturbations last about 1-1.1' days. @his differpnze
i
in duration indicates that the corpuscular stream caused @y a fl.-,re 1.9
liheterogencous and ganes ejected from the sun move at different apeeda.
IAn attempt is made to determine the aLream thickneas. A ahell including.
Ithe stream cloud is determined by the outer and inner radii. The differ-.-
itence between the outer and inner radii yields the dimensions of the
Card 1/2 UDC: 5@O,31L5-------

i ACC NR3 AP6032*684
;cloud. The beginning of the sudden magnetic storm indicates the
larrival of the first particles ejected from the flare which influences
I
;the radiation belts of the earth and the magnetosphere. This moment can
I
;be detected by the appearance of the D,t variations in the horizontal
!component of the magnetic field. D,t variations appear distinctly in
Irec-ording instruments of magnetic stations of low latitudes and have a
global character. When the D,t var@lations diiap- uar and t4e
;magnetic field is restored, it also means chat slow particles have
Ipassed the earth's orbit. The thickness of the particle cloud can be
.determined from the beginning and the end of the magnetic storm and the
Ivelocity of the particle stream. 'Moments of the beginning and the end
lof the storm can be determined, taking into consideration magnetic
lindices K, ap, and ac. K characterizes the general perturbed field, a.
specifies irregular changes of the magnetic field associated with D,t
!variations at low latitudes. and a. the same kind of changes in polar
iregion's. These indices characterize the commencement and end- of -the
!storm. Orig. art.-has: 1 table, 2 figures, and 6 formulas.
!SUB CODE: 03/ SUBM DATE: 17Jul65/ ORIG REF: 003/ OTH REF: 003
Card

KUSMI.P.I.. doteent
ftrl@
Heat effect of air temperature in sines. Gor. shur. 122 no.2:
36-37 F '48. 0CMk 8:9)
(Kine sanitation)
i

tr
*
qqqtf,f fill T11%itt wllt w I I Owe F6 W a
O
@
A r_G A 1- -4. 00 fA
,
1
f
k 4
"
"
ti; 4 , -
.. ,
'. i. 00
00 00,
00 00
00 852. SUMY OF ArR TO CWUCATED VFNTIIATING SYSTFMb BY NATURAL "00
00 t
@tol P. 1. (Gorr4rl 2mrnal (Min. J.), 1949, (9), 19-23).
j DRAIGHT. M
-so
00
Explanation of the use of grapb1cal wthode for finding the
00 uant1ty of air passing through aine workinge by natural draught. "00
0 0 _00
X,
.
Ji
000,
-00

:0

Is 0
00

v 0
it
v 0
4 - i L a Oky
ALLUVGXAL LIMATWe CLOSIFKATION '00
@

U SS tv -a a
a 0 t, a

a kajif WIC fft MMAJURML =1 W11CLUNAl IkAi 144 All,
.1.. ifill'. J.). 11.v
lv@WGU'4@ of Owot lZMAI@n 14 It
rj-1UlV 04) IM91`111 tJ tSWO *.1L3 Un th6 Quantities of swrful :*Uvt (I.Q..
;crtlclam Icss 10 c1cm4w) ;roduccl- In s"cific jcrattu4s. per
ratrs off n4c -'rilled. ;*r tan of Orr, bLUtse. cr ;.or ton InWed. rems-
urine av sw;,Ilng Whom to be w4c, 14 this ow. are .1,iscuszc-,. (L).

1. @rr-STIMIJI P@, I.; YMOMOV, V. K.; MOAS'TUI, B. P. mmn. (Reviewers)
2. USSR (600)
4. Mine Ventilation
7. "@Iine Ventilation.* A. Kh, lkaaokhov (author), abr, zhur. no. 111, 1952.
9. Monthly List of Russian Accessions, Library of Congress, January, -1953. Unclassified.

P. I.
I ampling Eethod If or t@-, -et@rir.@ tl at. Lon -o,' !.Io -A.!A i )" t@_
in Yin-s. I'inno Delo 1/3:0:k,@r "c"

Name: U)STIM-1 P.-vol Ivanovich
Dissentation: Experimcntal Stuly, Theory, and Calculation of
the Ventilating Resistance of Circular Mining
Shafta
Degree: Doc Toch Sci
Affiliation: Z-not indicated-7
Dofurux, Date, Places 25 Jun 54, Council of Loningrad Order of IA-n.Lr
r-,nd Order of labor Red Banner Mining Inst
Certification Date: 15 SOP 56
Source: BI.IV0 6/57

-T
IGNATENW. Koastantin Pavlovich, gorn.inzh.; BRAYTSZ'V. Andrey VasilIyevich,
kand.tekhn.nauk: VHYTS, Yelizavets Grigorlyevna, gorn.iazh.:
otvetstvennyy red.; GRISHAYENKO. H.L. red.izd-va;
AIADOVA, Ye.I., tekhn.red.
[Mine ventilation, illumination. fires. and rosette work] Rudnichnaia
ventillateiia. osveshchenie, rudnichnye pothar7 I gornospass tell nos
delo. Hoskva, Ugletekhizdat, 1957. 247 P. (MIRA 11:3)
(gins rescue work) (Mine fires)
(Kiae ventilation) (Kine lighting)

-MUSTELIP P*I.-
Determination of the coefficient of ventilation resistance of round
mine shafts. Zap. ILI 38 no.1:8-25 1959 14:3)
(Mine ventilation)

V
MUSTEL19 .I.
Determining the coefficients of rese.ve air in coal mines.
Zap. ILI 38 no.1:26-38 1959 Ca:@@'. 14:3)
(14ine ventilation)

INTSTELIS P.I..
gffectiveness of measures for reducing air leaks in mines.
ZaD. LGI 46 no.1:12-21 '62. (MIRA 16:6)
(Mina ventilation)

-,H1USTEL1-,-Pavel Ivanovich; DYATLOV, V.I.# inzh., retsenaent; YM4AKOV,
ZAYTSEV, A.P., otv. red.
(Principles of s&fety engineering and fire fighting tech-
nology in prospecting] Osnovy tekhniki bezopasnosti i protivo-
pozharnoi tekhniki pri geologorazvedochnykh rabotakh. Moskva.,
Nedra, 1964. 183 p. (MIRA 17:11)

BANDRIKOV, G.A.; KRASHUMMIN, P.Te.; RRYKHRUDEL. X.M.; POTEMKIN, T.T.;
MUSTALI, Te.R.; RZHMIN, K.S.; ITANOT. I.T.; KHAHLAKOT. A.A.;
TIKMNOV, 7u-.V,; STRAIZOTA, L.P.; KAFTSOY. L.N.; ORDANOTICH. A.Te.;
KHOULOT. R.Y.; VORONIN. B.S.; BXRMOVSKIT. G.N.; KRASKOPMSKT.
Tu.T.; KINAKOTA, I.I.; USTRENSEVA, T.N.; SMNOT, A.A.; WIND-
GRAWYA, M.B.; KARPXYZV, G.A.. DRACUT, L.A.; TH&IXOTA, N.B.;
SIZOV, V.P.; HZHEME. S.N.; VELIZRANINA. K.A.; NWAROT, V.S.;
SPIVAK, G.T., red.; NOSTREVA, I.A., red.; GBORGITEVA, G.I., tekhn.
red.
[Special practical manual in physical Spetsiallayi fizicheakii
praktikum. Moskva, Izd-vo Hoak.univ. Vol.l. [Radiophysice and
electronic@] Hadiofiziks i elektronika. 1960. 600 p.
(MIRA 13:7)
1. Profesaorsko-prepodevateliskiy sostav otdeleaiya radiofiziki
fizicheskogo fakullteta Moskovskogo gosudarstvennogo universiteta
(for all. except Spivak. Nosyrevs. Georgiyeva).
(Radioactivity) (Electronics)

2-IL875 S/109 /61/0CD6
D2627D- 36
AUTHORS: Braginokiy, V.B., Dianova, V.A., and Yustell, Ye-R.
TITLE- Inveatigation of the operation of a
plier using the non-linear capacity of
junction
iERIODICkL: Radioteklinika i elektronika, v.
117-.-: - 1177
L , I--eJ e T
4'E,@T: The above problem vias ir_IvCst_itrate-_' for cf
muil-i.pli-2ation (up to n @'-;.an scheme Of Th".
6i,ien in Z. The mul.tiplier consi 'sts of a 10 OiIL'
and a standard coaxial - %-.,z,.ve@,,uide pa!'@ "L;e. In ""Ie '_au zi 1.1il-l'od,
d_@ode 1, with its non-linear capacity. AY., a _@ I
from a generator (frequency range: 184 - 60u i::;
the input of the multiplier through a consta.,A 0 (.i L
db). 1.,aximum -,ower fror.. thL generator: -@.5 W. Co;:%Xi--'
@he non-linear element form the i-riput contour.
Card 2/5

24875
S/109/6-Li
rr,vestig,ation of the . . .
ted from the outside tube of' tiie, oo;_@.xia_'. Tne ou-.t)!@- iS
formed by coaxial piston 3 and two quarierwave Ibcai@-,-,2 J. Thr,:,ugh
a diapnragm it is connected with a r-rtajiguI-_r
filters oat the harmonics of' a .1, orvuopuridi. rig n-riiiiii.. '21x
tor of the resonator is 200, which -educes ne@100)at`lnr: Ilarilo-
nic,s vvith 20 db in comparison. Without fllter:zng, 1 rmon4!cs
times smaller, than the chos@,n @:_---rmon3.cs@ The (,utlu- oi:_..al
is fed into a spectroanalyzer, specially calibratec .:--Dr -lowir.-r, or
in-o a standard power meter. The output power cf 1@he :.,ui i @. (! - 4L s
snovni E-Iraphically as a function of the number of harit:or - in ',-, u t
z,i,,,,,,nal changed from, 184 to 600 1.!cls, output signal (9-30-11 and
input power remained constant. The ordinate represents the r:,tio
r-f the output power of n-th har;:,onies Io if the !9-.,h
-At -Input power P - !,)(J-J@C; M%/, LhC OUUPUL @.oviur jaturute@', I.,ere
for Smaller Coeff ciciii.E of L@Liltipl_,c tic)n. ?or --he invest4-.,tion
of phase stability 21 identical i,'lultil-liers were used, %vith tt,lo
vaives and ,.,easurin@; line of the sare direction. The
from a common C_enerE@.tor. After l'j'; hours of v;aruiing, a,,, i,@ v I- C e
Card ;/5

24875
S/ i091/61/006/007/015/C20
Investiv,@@tion of the D262/D306
was working for 9 hours without brezk. Phe amplitude chan@-ei @y
11) Change in )Lase differe-i-ce vi,,,@.q less than 60". To
of it,._orla,
wa.@@ ted -,n@ ,.C til-
p6nerits, fro@ @Ail-r. Wili,
I ine into _.oid
lar-.,c@ modul@t Jon it i.: pcls,-@ble to f7 -1
@Ije -ent.rai line and @@hc Side cor;,,.cnent.@.
povier: 2.5 mld (n (RzC)
"he irjp,,I@ power relng. of i,e .)f 21-k-) 1.11
tr--ai&formation loss v,,as n.)- nc;-e *han 1_(@ jl,,. a:i-_:i
Tnar, the m@.nlrrium. loss
Llys,@L, on -1,e
s -i s e d. w -, th an -_ @I c; a-, C
coe-@fl-ier,, 0, ... ... ond
,juvier LLre siiji@-@iy
Thic _n
hi;,,h-atabii@ty
-onstant of v)-n -.ur,-.,on of -@ne din(@e sn(,@iid bf_:@
,_ 12
i . 13 su--. There are r- r,@ E and nk2z,: - So v I e -. -6oj .2 fr.- n
Card @),, 5

2',875
Investi.gation of the D 2 e2li"F
ces. The re f t@rences to the .4 mk,,,@ recen t En,-, i oh- I c!-
ions read as f ol was . 1". ff. FL, flar.:i,)nic Gen, i -A e V.]
rr:c tif 1 ers, P-roc I, R. E. 0. 1 " @8; D. Lec rt--- A. III ir,
J Geri.-,at 1 on S 1) 1- U, ,.) e r. -
i e 6 VI i t @ I " - r, ,-i 1, -, -:1.,: d i c) rI e sPr,; 1@ 19@9f LU. 4 D. 71
'j
S. Vieirreb. Fre@@-jen-,y -:iui vi-tli nen zapa-
--lt@ors - A r4rcuit analysis. Pyo-,- 1-1 2()'7'-. R.
Lowe-11, E. Kiss, Solid-staie i:,i,--z-ewave uovier sources r: - o n
@Leneratlon, Proc. T.R.E... I@bC), -, 1834,
A@3:30CIATION; Fizichesky @@'a4u-' @ T.-@ 11-!ocko7isicogo gosudar-6:venn,-q;u -Ani-
versite',a -cr,, LC.--,orosova, rLafedra teciri kcl-@Jba-
niy (Fucl@ltv of P@,, r,'os(-ovi S)tate
T,.V. Loioncsov.. ljt2par,@ment of Theory of Os:@-J -'-- llion@-)
SUBMITTED: T.'ovembtf- 17, lljr'jO
Card 4/5

@1075
Investigation of the S/109/61/006/007/015/020'
D262/D)06
Fig. 2. Main scheme of the construction of the multiplier.
Legend: 1 - Non-1-inear capacity; 2, 3 - coaxial Distons; 4 quar-
ter wave beakers:, resonator filter.
7, @k ,,J @,A,,
jj I.-I "
Piic,74' r1payujiumanwian cxeN%a i(oucT-
JIA:
pyl(IXIISI YNIHOH(Iffe
HeAHM(Waff e'4HOCTb; now(cuanhimw
- P- 8!
noptutut; j - ReTsep-Tha@olloaue cTaltaHu: f
SwInTOP-OunwrP
Card 5/5

S/ I @' 9/ 6 2/0 02 C,
9, D25 6j/ D3 rV' 7)
AUTHk., j: Dianova, V.A. . Maneshin N K . LaLe-L- Ye R -nl
Parygin. V,.N
TITLE: UHF-multipllier with a hIgh M11.1''
PERIODICAL: Radiotekhnika i elektronika; v. 7, nr-, 2.1@6_
348 - 349
TEXT: Preliminary results are repori@ed on inve,--tigating R
multiplier with a p-n diode used as a non-linear capacity rhe 7rn-
struction of the multiplier was easen-!,ially identi-,-,all To rna@ ie6-
cribed previously by V-B, Braginskiy, et al. (Ref- 4: Radiiotekhni@ca
i elektronika, v, 6, no@ 7, 1961, 1173), but the oatpu-, freqa,?n_y
was increased to 24,000 Mcs/sec. The depen@ence of zhe o,Atpu7 power
upon the number of the harmoni-- is presenled in ,he form of a -ra@h
showing that between the 32nd an,! 85th harmonics the power de-rep.-
ses smoothly by 14 db, The m,,ximum signal obser-red was 'i it above
the noise level, The time constant of the diode measured a-, - If) V
was 1,14 x 10 -13 sec. Ai, 660 imcs/sec input frequency the
Card 112

UHF-multiplier with a high D25b/D303
was found to be adequate for heteroayne purposei--, and -.t vr,s A-@ed
successfully for re,-I-raing sIgnals from a T L e -
re are 2 figures and 1 So%-iet-c!I,)- refer.-@.,-.e
ASSOCIATION, Fiz1.--hesk:y t", Mosk@jvsic--,,@g--
universiteta im. W V L-Dmcn@-,@,Dva
Moscow S@ae Univprsity in V L,--!nn
SUBI"TITTED: J--ine
Card 2,12

S/10 b2/(-')07/,C, "'I"
D271%302
I.:us tel Ye. R. , and Solov I yev, -a.
-2 7-2 '-he use of coupled resonant cLvfties in Je,----.,i@
-ode as microwave band-pa-ss filters
;@ad.J'Lote'-IIIni'r-I@-. i elelctronika, v. 7, no.
710 - '115
1,esulis are -reported of ar exporimen,@a' s-,u@, of
of '0and-p-ass filter for the 3 cm band, with a TiLx4LixU;.-,
76 L-c/s. '@:he disturba.-.ce of the cavity in vih_'ch
7-ace couples oscilla@ions of vL-rious modes ,7hich h-.vQ C).,
vcry close frequencies, i.e. t-.e degeneration is
C&v-ities wit1i n-fold deCenerLtfon are coupled, the syst."m
analo@;ous ta 2n coupled circuits. '.Phe filte.- VI-tich @-.:@as S*.,.;(,_-_,@-!
s'.-_ovTn in ?iE;. 2; n was made 2 or 3. Attenua-Lion measurc-en,si,
subs--itution, were performeo, with various couplin@@ dia-p'..:-a(-:..,;; C
vities were disuurbed oy screws and their Denetration
so as to obtain minimum rippie witiin the widest nossible .h,
cou,oiir- ben@ieen two difrerent modes, with identical or ne_---i-.c:@-@i_
C r C1 1

The use of coupied resonant c_@vitles ... D27-,/D--)'02
cal frequencies, is expressed by in ter-mo@@e coup_;_i-,,- cr,@!:'f
ffifT. V , V - - V
Ij V -i-j j
4-
In a fl@ilter `.-oui)-7c der-enerat-ion, op i-,, .o
a-. 4DO or 1350. The loaded @-facuor of cavi-@_Jes
_ener,@_.tion was 600, with tripie ae@-,eneration - 50G. 5
L
_.ioii improved very cons id, e.',LDIY both the band-viJi'@h -,n
..-steepness of t.iie systf,,@.,,. Triple degener,%tion occil-s 11or a
-ela- wher - 0-)
uion o.17' cavity dimensions, e.g. 1/a :- 2. 2 , H
71 17,, ve all the same frecuency; two scre,.-:s --.fe
-a
and f.-equency characteristic.3 are civen for
:-_nera-.ed fil-.ers wIt. %r@.rfous 2-4aphra,@:.-.s an(! scre-:1
T', e s y s -,. e mm , w i -,, h b ee r @4'- f a c T, o _- o f ca v J. t i e s , c an lIze.-I
ci,,@enc- detectors. T*n-ere a-2e :5 igures, 2 tabless an@@ 6 --c.-fer
Qov.a.e-,,-bloc and 4 non-Soviet-bloc. The references lt:) t,,@e
lan,guage publicutions read as follows: A.G. Li-.,,le, Pr@;c-
4 9, no. 4 # 10,61 , 821 ; G. Shaf fner, and F. Vcorhaar, P:-,:@.
Card 2/3

SOURCE CODE:
6014255. 9166/011/005/0947/0949
V
DiAnova, V. 4-tatel,_,je. R.; rtir@ in
ph@ -loscow State University im
ysico 'e ar ment 0scillation'rhysics Seaiati. t
M. V. Lomonosov (Firicheskiy fakul'tet Maskovskogo gosudarstvennogo universiteta.
edra-f i'iik: L'.1janiy)
TITLE: Light modulation by 3.2 cm wave
SOURCE:f Radiotekhnilca i elektronika, v. 11, no. 5, 1966, 947-949
TOPIC TAGS., modulated light, optic modulator
ABSTRACT: An experimental inve 'stigation of light modulation was made aL a frequency
of 9260 Mc using the linear elecLro-optic effect in a single ADP crystal. A cyl-indrl+
cal resonator, in which E010-type oscillations were excited, was used to produce the
required longitudinal electric field. To reduce Ims-m due to ubf and to Increase the
modulation efficiency, the resonator was partially filled with an electro-optical
medium. A crystal, 3 mm in diameter and 10 mm Iong, was used for this resonator.
ht modulation was accomplished in a pulsed regime with a large duty factor. With
.9
-.--a.145-w mqdulating power a phase shift of 0.46 was obtained, which in turn corre-
spon ded to a modulation depth of 44%; with a modulating power of 9 w the modulation
3 rad2jw.
..-depth Was 12%. The quality of the mbdulatbr for such 6 system was 1.4-10-
1%.-Card 1/2 VDC!. @35*24LD

L 261148-66
ACC Wt AP6014255
A modulator consist ing,of two identical resonators with ADP crystals was also in-
vestigated, Both resonators were excited by the same generator. An increase of 1.75
1.11 the phase shift at crystal output was obtained for the case of an optimum phase.
A shift in the uhf field phase by -a from the optimum phase at wavelength X - 3.2 cm
reduced the modulation depth to zero. This confirmed the fact that light modulation
actually occurred at..X 3.2 cm. Orig. art. has: 3 figures. [JRIJ
SUB CODE: 09/. SUBUDATE: lliun65/ ORIIG REF: @001/ cylit REF.- (304/ ATD PRESS:

!ACC NR: AP6036381 SOURCE CODE. UR/0109/66/011/011/2082/2085
'AUTHOR: Dianova, V. A.; MuptWs_._Ya.._R.j Fishuk, A. P.
ORG: Moscow State University im. M. V. Lomonosov Mookovskes6gosudarst-
vennoruniversiteto-)
TITLE: Frequency c-mversion using double modulation of light
SOURCE: Radiotakhnika i elektronika, v. 11, no.- 11, 1966, 2082-2085
TOPIC TAGS. light modulation, frequency conversion
ABSTRACT: D. J. Blattner and F. Steraer proposed a system for optical-band
frequency conver3ion which permits using low-frequency photo detectors for
reception of SHF- signal -modulated light. The syptem comprises an electro-
optical crystal (frequency converter), an analyzer, and a photo detector. A light
modulated at frequency falls on a crystal placed in a field of frequency 40,;1
i_Card I /_Z

R: AP6036381
the resulting light afte r the analyzer comes modulated by combination frequencies
m W, -+ n "J. . where m and n are equal to 0. 1, 2. 3. A lowest
frequency is of practical importance. A further analysis of the above system
1 points up the expediency of a polarization modulation jinstead of AM); the polari-
I
zation modulation system is simpler (the analyzer and two .1 /4-plates not
needed) and promises a double efficiency of conversion; the same electro-opticaL
crystal can be used for modulation and conversion of frequency. In an experi-
mental verification# a resonator was excited at 700 and 701 Mc, and an output
signal of I Mc was received at the output of a photomultiplier. "The authors wish'
to thank V. N. Parygin for discussing the results. 11 Orig. an. has., 2 figuree i
and 9 formm-1-s. RCA itev., 19620 23g 3v 407-
SUB CODZ: ZO 09 SUBM DATI9t UFOW ORIG P"t 003
card a 2

DIANCYVA, V.A.; MANESHIN, N.K.; MUSTEL', Ye.R.; PARYGIN, V.N.
F@requency multiplier with non-linear capacitance and high Q
circuits. Radiotekh. i elektron. 9 no.6:1079-1081 je 164.
(MIRA 17:7)

CALIKOWSKI, Roman; MUSTER, Hanryk
Preliminary studies on the boring susceptibility of rocks. Przegl
geol 9 no.8:424-425 Ag '61.
1. Politechnika Warazawska.

prol
1'= tnoi
no.
r5,iw rxvir- OF @he i 3r, Astrcma,it @cal
Orietirman, Wa
We I-,;a-w.

Y/001/62/000/011/001/002
D267/D307
AUTHOR: Munter,_,Jg.@e., Engineer
TITIZ,: &xperimental production of pure synthetic minerals
in a solar furnace and their characteristic features
FERIODICAL: Tehnika, no. 11, 1962, 2091-2096
TEXT: The e=13crimental solar fVn-nace, erectecl by the
(Slovenian) Mlctallur,,ical Institute of Ljubliana at Piran in 1960,
is describ8d in detail. Local conditions permit temperatures of
about 2500 C to be attained during 150 sunny days everv year, and
up to 2800 - 29000C on some days in May - July. The lieLiostat has
an automatic motion controlled by photo-transistors and a hydraulic
driving mechanism. Usual porcelain crutibles can be used since the
mixture is fused only in the center of the top layer. The minei-als
were obtained from two or three of the following oxides: CaO, MgO,
A12031 Si02' About 0.5% of carb'on black was added to the oxide mix-
ture in-order to facilitate the fusion. The following minerals were
synthesized: dolomite, corundum, spinel, anorthite, cordierite,
Card 1/2

Lxperimental production
Y/001/62/000/011/001/002
D267/D307
wollastonite, 0-rossularite, 1-teleni-te, akennanite, forsterite, 11onti-
cellite, shannonitc, menrinite, mullite, clinociistatite and diopside.
The quality of ten of these 16 minerals was excellent. The identi-
fication was carried out by the Debye-Scherrer method and by means
of