DETERMINING THE SIGN (POSITIVE) OF THE CHARGE OF PRIMARY PARTICLES OF COSMIC RAYS BY MEASURING THE AZIMUTH ASIMMETRY IN THE STRATOSPHERE IN THE REGION OF THE EQUATOR

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP80-00809A000600270167-7
• Release Decision: RIPPUB
• Original Classification: C
• Document Page Count: 3
• Document Creation Date: December 22, 2016
• Document Release Date: September 15, 2011
• Sequence Number: 167
• Publication Date: December 5, 1949
• Content Type: REPORT

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CLASSIFICATION C:uiV.pi1 1 flAI e T i , ia~Ir*
CENTRAL :Nri-I_LIGENCF AGENCYPORI
INFORMATION FROM
FOREIGN DOCUMENTS OR RADIO BROW: "A.STS CD NO.
PUBLISHED 1 Jul 1949
LANGUAGE Russian
DATE
WHERE
PUBLISHED Moscow
COUNTRY U93it
SUBJECT Nuclear Physics - Commit rays
HOW
PUBLISHED Thrice monthly periodical
11-11 OOCYYYNT CNTIIN, 14111MAM" """MI TYI NA1IO111 ^116X8:
OF Ut MUD ITAT11 .1M. Tki YUMING OF IYPIONAO 6T p0
Y. : 11 AYD lt, AY "t-KO. IT$ OR I.,
THIS IS UNEVALUATED INFORMATION
Emmmm T!#S SIGN (PCSITIy) OF THS CHARGR 08 PRIMARY PARTICIiS OF COBif,IC
RATS BT) AS RING TIN AZDIIJT ABTII~E'H$f IN TM BTHAT08PHSRR IN THS
EM ON OT TER NQULTOR
S. N. Vernov, H. L. Grigorov, N. A. Dobrotin, S. P. Sokolov, B. D.
Savin, and A. I. Surakin, Moscow State Univ !rani M. V. Lomonosov
and the Physics Institute imeni P. N. Lebedev, Academy of Sciences
USSR
C Digest)
The charges of primary particles can be de`~rmined as to sign by mea-
surirg azimuth asymmetry in the stratosphere near the mag otic equator. The
presence of this asymetry was ppoved by Johnson, Rossi, and borff (1) in
their study of the vest-east azl*ath asymmetry at sea level and on mountain
tops. However, no defipite conclusion. resulted from these experiments on the
sign bf Primary particles and their nature since the particles reaching the
measuring device in thesp experimemki. were of secondary or even tertiary
? derivation. In order to decrease tie influence of secondary processes upon
the azimuth asymmetry, asymmetry must be measured at b%b altitudes where
primary cosmic radiation makes?up a lubstantialpercent of the total number
of particles. Azimuth asymmetry in the etratoepuere has been measured by
Johnson ant Barry (2). Their measurements revealed practically no azimuth
asymmetry at altitudes of 20-25 kilometers; it constituted 7 percent, whereas
it shoulihave constituted 60 percent all the primary Particles has a pos-
itive charge, according to Johnson's calculations.
Johnson, from hi,s experiments in measuring azimuth asymmetry at sea
level, concluded that all primary particles are positively charged, i.e.,
are protons. The very small azimuth asymmetry observed by Johnson in the
stratosphere is'expiiined in a number of works by the fact that secondary
particles do not retain the direction of primary particles. A. M. Lu ilov's
cx rimants, i'op,ever, nn iiad that the dispersion of eecoadery particles
is small and does not even come close to a value capable of decreasing azimuth
aeymetry from 60 to 7 percent. Thus, from Johnson's and Barry's experiments,
taken together with those of Sulikov, the conclusion follows that particles
STATE
ARMY
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SUPPLEMENT TO
REPORT NO.
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with negat 7e charge make up a high percent of primary cosmic radiation.
Moreover, these particles cannot be electrons since S. N. Vcrnov'e exper-
iments (with collaborators) (4) showed that there is no noticeable number
of electrons in the composition of primary particles. Consequently, we
must admit the existence of negative nonelectronic particles, i.e., hypo-
thetical antiprotons.
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g na r of
e
the photoelements. The relay then opened the circuit to the motor and rotation
of the telescope stopped. In this fashion, a definite orientation of the
telescope with respect to the sun was maintained. A correction for the change
in the azimuth of the sun was provided for with the aid of a small time meohar
nism which turned the photoelementa.
The accuracy with which the fixed direction of the telescope was maintained
at sea level was 2* 15 degrees, and must have been much greater in the strato..
sphere because of increased solar intensity.
In addition to the triple co!ncidencee selected by the telescope, the
number of showers was also measured simultaneously in the unit. This number
characterized the shower-forming properties of the radiation coming from the
west and east. The showers were registered by a four-coincidence circuit,
which was triggered for simultaneous discharge in counters 1, 2, and 3 of the
telescope and one of the other counters.
n
e e instrument suspei,ed in the sounding balloon
rotated in various directions during flight, it was necessary to maintain
the telescope in a definite direction alternately, either east or west, in
order to measure west-east asymmetry. This was achieved by fastening three
photoelementa"firmly to the telescope. The planes of two photcelemahts were
parallel and placed so that sunlight could fall on only one of the photo-
elec. ants. Each of tt:_ phn4toelements was connected , iwitt the grid of its
tube, whose plate circuit included a small relay. When, dme to the rotation
of the unit, sunlight fell on one of the photoelementa, the relay was
activitated, and its contacts closed the circuit to a small electric motor.
The electric motor turned the telescope until the sunk ht fe11 o
ith
Thus, the sign of the charge of primary cosmic particles remained an
unsolved problem. In order to solve thde problem decisively, we devis6d a
special instrument which was lifted to the stratosphere in sounding balloons.
~l'he basic part of-the instrument was a telescope inclined 60 degrees to thb
*kertical. The number of particles counted by the telescope was transmitted
by radio to a receiving point, where it was recorded in the same manner as in
previous works (4) Si
c th
The resolving pC pr (time) of the triple-coincidence circuit was b - 1076
seconds; the resolving power of the tour-coincidence circuit we t = 3.10'
seconds; Every guadruple coincidence was recorded on tape at the receiving
point.
Triple coincidences operated an electromagnetic indicator with an arrow
on a disc having contacts. When the electromagnetic indicator had counted a
definite number of pulses (90 in the case of telescope without lead aid 45 in
the Case of a telescope with lead), the telescope was rotated through 180
degrees,i.e, from west to east or vice versa, and this position was maintained
in the manner described until the electromagnetic indicator had counted a
definite number of pulses; after which the telescope was again rotated through
180 degrees, etc. An audiofrequency corresponding to each position of the
telescope was received at the receiving point; thud the time the telescope
stayed in the west and east directions was fixed at the receiving point.
This also made it possible to determine whether the automatic device for main-
taining a definite telescope direction was operating correctly.
IrI~
L. il'v E, 111 .c'.~
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~' Azimuth asymmetry was measured on board a Diesel-motor ship at geomagnetic
latitude 6-10 degrees south. Five inetrmients were sent up, three to measure
the asymmetry of total intensity and two with 8 centimeters of lead between the
te'escore counters to measure asymmetry of the hard component. The instruments
flights agreed well.
curves being the averages of three flights. The curves for intensity of the
hard component in west and east directions were shown similarly. The points
are the averages of two flights. The amount of matter (thickness), in grams
total intensity, reaches 45-50 percent at high altitudes. The azimuth. asymmetry
especially apparent from the high asymmotry of the bard component.
As was iaviicated previously, these same instruments also measured with
respect to a3. ee the behavior of showers caused by particles of the hard
ocmponent. The reswlts obtained indicated a substantial difference in the
a titndtna behavior of showers near the geomagnetic equator sal at A latitude
of 50 degrees North,
Thug, our experiments established the high east-west asymmetry in the
stratosphere, which proves that the charge of primary particles is positive.
1. T. H. Johnson, Pbye. Rev., 43, 634, 1933; B. Rose, Phys, Rev., 45, 212,
1934; S. A. Korff, Phys. Rev,, 44, 515, 1933.
2. T. Johnson and J. Barry, Phys. Rev., 56, 219, 1939.
3. S. H. Vernov ani A. M. Nulikov, Alfa, 61, No 6, 1948
4. S. I. Brikker, S. N. Vernov, I. M. Tevreynova, S. P. Sokolov, and
T. B. Qharekch'yan, DO, 57, No 2, 1947.
Y~~jf riu r.>i i11L
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