(SANITIZED)SOVIET PAPERS ON SPACE AND UPPER ATMOSPHERE RESEARCH(SANITIZED)

• Document Type: CREST
• Collection: General CIA Records
• Document Number (FOIA) /ESDN (CREST): CIA-RDP80T00246A022400050001-7
• Release Decision: RIPPUB
• Original Classification: C
• Document Page Count: 165
• Document Creation Date: December 23, 2016
• Document Release Date: December 13, 2012
• Sequence Number: 1
• Publication Date: July 12, 1963
• Content Type: REPORT

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STAT
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AURORA AN:I;Ti AICLO
V.1. ea A s o v
? ? y
.Ictitutof atmospheric PhyJics, Academy of
L;ciences, USSR,
Principal facts on the aurora and related aire-low are
described. The paper con4ains ,..1c.)me critical remarkw and
Outlines.
the necessary objectivos of further reaeilr,:h.
It is generally recognized.' that emissions or upper
atmosphere are caused mainly by ?three factors. Firstly,.
by variou-s chemical reactions. Oecondly, by the excitatiom.
of molecules ansl atoms of at=sPheret.lin the process of
colliding with other energetic neutral: and charges particles.
.An.d thirdly, by fluorescence of setae 'atoms and molecules of'
titmospherepincluding metastab/e particles, in irradiat?
ion.. The most intensive eMissions of upper atmosphere are
observed during.thecaUrora. Eigh'sensitivity.of modern
? spectrographic and eiectrQ?piioiometr4c,apparatus makes it'
possible to register typical omissions of very w ak aur;Jrati
which can be neither-observed visually nor p!;oto7raphed. The
number of such.aurores le '4uch-greater coMpered with thone
detectable visually or photographically- They are observed
not onlyin high?latitude areas but in low? latitude and.
equatorial areas as well. [1, 2, 4] . It'is not improbable
that the ,introduction. of electrophotometric and spec tro ?
graphic- apparatus of higher resolving power :sensitivity
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?
will make aurorea a uraual phenomenon oily obaervud in all.
:reogions, and the attribute "polar" then certain to
looe ite' absolute moaning.
So far the main data on aurora have been obtained r
by meana of ground observations at night in visible and
near ultraviolet 'and infrared areas of the spectrum
[4, 5,60 71 . Highly desirable data on emissions which
do-not penetrate.the earth' s atmosphere c> uId be obtained
with the 1-Mp of rockets and sputniks. Unf)rtunatoly,little
,hau been. done in this respect. The absence of regular data
on aarores in the day?time is also a conaiderable dieadvan
tage. The proppects for the uae of rockets and oputniks in
order-to eliminate the masking background of diffuse
atmospheric light are very attractive. However, these
possibilities remain absolutely uneIploited.
The phenofzenon of aurora is associated with addition?
al ionization of upper atnosphere.. If the energy level
-of the. exciting agent is higher than the -ionization potential
of atmoapheric mo/ecules and atoastthe optical excitation
is always accompanied by ionization. This ionization can be
detected with the help of ground radlolocati on of aurora
[8t.
The picture of the distribution of ionization and .
radiance is in senora/ rather consistent eapacially if
we have in mind the 800motrical conditions of radiorenect?
ions and the fact that the average life of eacited atoma
and.bolecules responsible for radiance is much shorter than _
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?
the average life of ionization which ensures the diffdeion
of electrons and ions from th, place of their origin to
the neighbouring regions of the space. If an exciting
agent which is able to penetrate below tha 100 km level
appears during aurora, the ionization of this area is
accompanied by additional absorption of radiowaves'both
a
?from terrestrial andspve sources [4,5 101 .
The ground observations have shown that spectra of
aurora, appart from absolute intensity, are characterized
in the first place by the relative centent of atomic and
?molecular emissions. This ratio is highly variable and
evidently reflects the depth of penetration of the exciting
agents into the earth's atmosphere. The deeper is this
penetration, the more intensive are the molecular bands and ,
the weaker are atomic emissions, especially from metastable
?states. The energy of the highest levels of radiating
? particles is another characteristic feature of emsisions of
aurora. ?Luring many auxores high levels are excited with
an energy of tens of ev. It is natural that such exit-
ation is accompanied by intensive ionization of the atmos-
phere. It happens .? however, that spectra of aurora
? display abnormally Intensified metastable emissions of atomic
oxygen and nitrogen 6300 a and 5200 a (excitation
energy 1.96 and 2.35 ev respectively), ?sometims even
without traces of other emissions from higher excited levels,
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for example, even without incrvased metastable emi sion
of o..,.agen 5577 ?C. (excitation energy 4.05 ev). And ,
finally, the most rezarkable feature of the spectra di aurora
is the presence or absence of hydrogen emission with a
wide spectral contour. Zhenever the radiation proceeds
from the magnetic zOnith the contour of such emission is
always shifted .to the short?wave part of the spectrum. The
wide contour of hydrogen emission can be most easily ex?
plained by the penetration into atmosphere of comparatively
soft protons with a rather stable wide interval of velocity.
The meet frequently encountered velocity corresponds to --an
energy of about several hundreds ev, [7, Only in
several cases has a contour corresponding to about 100 ev
been observed [12,- 131 0 The most intensive hydrogen
omission with a wide contour is more often observed in
spectra of atomic type though very often it is not obserrid thereat all. It iu necessary to.point out, however, that
radiation of the night sky is always accompanied by weak
? hydrogen emission H j with a very narrow contour which
corresponds to hydrogen atoms with an energy which does not
exced several tens of ev [4] ? The origin of this
emission is not completely understood yet. 'Olen aurora appear
in a sunlit area they are, supplemented with fluorescent
emissions of the ionized nitrogen molecule arid metastable
orthohelium atoms 14, 141 4 '
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These peculiarities of spectra of rree nable' h
conclusion to be r.ade that in some caoes.but by no zaans
always, ewissions of aurorae On be excited by faat protons.
It is interestin to note that at this time some relative
?
weakoning of the l!einel aystem of the ionized nitrogen
molecule and somA relative inte$seification of tho omission
of ionized nitrogen about %)04 are.obe2rved. The same
peCuliarities are observed in experimentally produced
spectra with oimilar exciting agent;. when vary fast
protons are able to penetrate into ,lowar areas of atIzosphere
with molecular composition, hydrogen emission may be hidden
from observation be.erue of intent-sive 41.indina wi th bands
of netttral tuid ionized nitrogen molecules. When. hydrogen
emission with a wide contour is absent aurora can be excited
by fast electrons. The energy of primary protons and
electrons responsible, for aurora can be de,termined approxi?
mate' ,by tho lower margin of giow. .1n order to penetrate
into the atmosphere below 200. kin the pr.iraary proton should
have an energy exceeding 05 key, t.Ao primary electron ?
only above 20 ev. In order to penetrate below .10) km the
energy thresholds exceed 200 kev and 10 kav rapectively.
Zmissions of atomic type are usually obsrved at highte
exceedinz 200 km. The lower border of bome auroras lies
lower thnn 100
- Z..Om e Amarican:scioGtists have used rockets to
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investigate corpusclos which caus,:: aurora' at he it below
200 km .0 1 ') 0 IG 171 18] ? Vz.v.-y have ,discoverea electrons
with energi of .aever'al key' arid protons with energies'
or hundroda of key. As tar ?aza electrons .are concernd ?
these energy date acx-ve w1ti'4, the. rsults or ground obl)erv?
ations. As to protona,ho,Never,their energy .ati:Lats are
? much higher than the low owls which ere ? 4!;xpected according
to the observed. .-Doppiar shift towards the hrtwave rt
o the pectrum.? it in quite possible that the obsycd pro7
tons did, not cause- aurora; the latter-verc then excited ?
by. protons with sheriri,:ia of: -several' hundred ev which ware
not regiztered by the apparatus u2ed? Apparently additional
inveatigati ohs should be undert .i.;zen to coilct more reliable
date.
The above";iaentionod invesfiaations have c.lade it
possible to establish a certain vqationship betw:n the .
radiance of aurora and priury corpusclea DC]. Thus
it ha u been estimated that about.0,1 4"4 of the primary energy'
of corpuscles turn into visible radiation, It is desirable,
however,to know thIa value more exactly ua a function ef
the height or radiance taking into account the back flux ?
of corpuscles reflocLed from the acne tic field. ,It is
very. important, to'invet3igat nimultahauaaly the enevay lost
on ionization, and the rdialion in spectrum r4;iona
inaccessabla for around barvations.
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? ?
It is n.,cessary to notelhowever, that the investigat?
ions which have bean -;ccomplishd, are not sufficient for
conc/usive determination of the nature of the initial
exciting agent of polar lights. since various mechanisms
of' the generation of corpuscles in the earth's 'exosphere
itself are beinc, discussed, it is impossible to deny un?
conditionally the existence of a corpuscular flux consist?
? ing of atmospheric ions N2F, N+, ?2 Ci I
.Nor, Ark, Re ). Besides ':;hklovsky admits the penetrat?
ion into the Earth's atmosphere of neutral hydrogen atoms
which are formed in the interplanetary space durin the
re?charge and neutralization of protons of primary cor7.-- ,
puscular f/uxes [191 . This process should augment in a
medium filled with micrometeorites. As to electrons with
an energy of several key the excitation of radiance should
not be attributed only to primary electrons. It can be
caused by secondary electrons which appear during atmosphere
ionization by primary electrons'. secondary electrons may
possess an energy of several tens of ev and, mixing with
thermal electrons of the upper atmosphere, form a surplus.
of primary electrons as compared with the value which
follows from purely Maxwell distribution.
. It is necessary to note that the energy of corpuscles
' (protons and electrons) found in the upper atmo:Jphere
does not Correlate with'the delay time Of the beginning
, of geomagnetic storms in relation to the appearance of
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active- formation in the Sun. ,This is a convincing proof.
that CorpS.sclos which couti:1 aurora are not primary solar ?
corpuscles but originate in the terrestrial, exosphere as a-
result of soma comples proceea of -interaction with
corpuscular fluxes or thc I3un. Of great inten,ist is the
abnormal intensification o metastable emissions of oxygen
and nitrogon atoms 6300 and 5200 a with a low excita?
tion potential (l.96 and 235' ev respectively) without
any significant intensificati on of the aletastabla emission
of atomic oxygen (5577 a ) with a slightly higher egcit?
ation potential (4.06 ev). Two mecanisma of such select?
,
lye excitation, of the abevementioned emission are -possible
in principle. Pirst of all, it ie excited by thermal
electrons-at a ttperature of aiveral thousand degrees K,
which. i3 insufficient for simultaneous excitation of
the gveen emission of atollic oxygen. This temperature,
however, is higher than the tmparature of 10GC-1200? K
which is usually expected .in the region of at.lrora. Another
possibility is selective origination of these emissions
resulting from chemical reactions, for example,in the proces
of diociative recombination of ionized molecules of oxygen,.
nitrogen and nitrozen Oxide [7] . .11owcver,whan molecular
emissions are absent and the intendity of the red emission
of atomic oxygen is too high such a mechanism does not s,iem
probabletfor it is difficult .to admit that there is a swift
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and abundant upward entraiment of molecular ions formed
below.withont the excitation of molecular emissions.
It is important to underline that corPuscles with
energies above several ev cannot be agents of abnormal red
emission of atomic oxygen 6300 i 0, If these corpuscles.
were exciters of the above emission it would have inevitably.
. resulted in other emissions corresponding to higher excitation.
:? This is not obserVed,however.,
To conclude
we must point out
oxygen that can be
our review of emissions of aurora
that it is only the red emission of
somehow explained by ch,::.mical reactie-ns,
for exampIe,in the process of dissociative recombinations of
molecular ions. J?Such a mechanism. ? however, is of no use for
explaining other .omissions with a higher .excitation potent
ial. During the cOruscation of aurora, in a period of
time less than a second all the principal emissions,except
the red oxygen. one 63GO a, have -a synchronous development
and equal relative depth ot modulation. since the time of
Ion recombination greatly .exceeds a.second this is possible .
only when the excitation. of emissions is the result of either
a direct impact of primary -corpuscles or short?lived second? .
ary electrons which _have originated from them D.:, 273.
? ? . We have suggested the idea Of sporadic ionization
and .heting or the upper atmo4vhese with corpuscular fluxes
and systems of ionospheric. currents,. assuming- expansion .of
-;
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the Upper atmosphere as a result of heating [204 21-, 22*
23 some authors believe -the heating to be the result
of magnetic?hydrodynamic waves [24, 25] Its has already.
been found with the-help or interferometers that during
intensive aurores With abnormally intensified. red emission
of oxagen the width of its Doppler contour teatifies to the
:rise in. temperature. Tomperaturea reaching 3500? K*
[26] have been .registered.
The heating la accompanied by an increase in the
height of uniform atmosphere and by circulation and mixing.
-.All this are. satisfactorily- .confirmed? with observationti
of _intensive aurorea. The upward .movement of a great
:mass of nitrogen molecules results in an increase in the.
number of their ions_ there. They are easily observed
beyond the Earth's ,shadow due to fluorescence which is
clarlyx .clearly seen thanks to welI?developed bands from
high vibrational levels of lens of molecular nitrogen. Thus*
for .example, on the 11th of 1?ebruary,19.58, when aurora were
studied in 2venigorod, at 300 to northernhorizon* at
altitudes of over 300 km there were about: 5.1011 ions
of .molecular nitrogen in the line of vision with the-scale
7
height of about 101 cm approximately corresponded to several
thousand N2t in cm3. It is necessary to remember that
the detection threshold was about 5.108 ions of N2t om?'
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In the line of vision and that under uaual Conditions those
ions could not be detectod. awing the aurora on the night,.
.from the 4th to the 5th of Novemberp1953, 1121: ions about
two ordoro lase itrnwabar were observed above the 500 in level.
Additional ionization and heating. of the::; upper .
atmosphere can be attributed ,even to weak corpuscular fluxes and,
systems or ionospheric durrenta. Tho additional ionization,
which was expected, by usoculd be the ceu of disturbance,
of the uniformity of ionoaphere and appearance of oporadis
layers. Later some authors argues in favour of a more slant?
?
ficant role of the processes 23, 293.. But such :trend in
the developMent of this idea encounters a Very. serious o1S-Stacle,
1.e. the absence of significant emiesions above 1.00km. Zome
non?uniformities of _radiation fields of thee night sky may also
be suspected as traces of corpuocular excitation. However,
the final solution of the problem requires an accurate deter',
mination or heights of those additional radiations. It is
highly importaat to .carry Out regular obssrvations of the
height or the initiation or emissions in ionosphere at
different latitudes and in different parts Of the day. ?
Systems of ionospheric currents are naturally aszo?
.0iatild with thefexistence of systems of electromotive forces,
These systems must change, movements and locations Of the
trapped corpUoclestespeciallgowbea energy of these corpuk;clos
IS small. The circulation of the ionized upper atmosphere
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in the geomagnetie field may be one of the causes f the
.existence of systems of electromotive forces. When vertical
electromotive forces of 4-definite direction developoupward
diffusion-or molecular ions is .possible. This phenotenon
as well as the expansion of the upper atmosphere upon.
heating. may lead to an exteneion of aurora in height.' We.
'have notices that the development of-aurora ia accompanied
at not only by fluorescent emissions of
ionized hitrogen molecules but also by emissions of metes-
-table atoms orthohelium [4, 14]. In this connection it Is
interesting .o note that as far back as 1952, Gartlein
[301 found that the appearance of nitrogen molecular
emission originates 60Mowhat later than the initiation of
polar lights. And what is more,already in 195 Gartlein
explained th'e, ?wel/?known phenomenon or the shrinking of the
?lower boundary and extent of aurora in height in the years
of minimum solar activity az compared with active periods
due to the diminution of the extent of the Earth's atmos?
phere it this period. [311
The nature of polar Its lights varies conaidertfoly
at different geomagnetio latitudes. We distinguish three
principal types of polar lights with regard to latitudes
1) polar area lights
2) usual high?latitude-aurores;
3) low?intensity visuall,.?unobservable lights of
middle and equatoria/ latitudes..
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7 13
Typical polar area iiit are caused by pro' ns
of solar origin with an, energy of several tens of a's,
[329 334 34] They reach' the Larth in 'several tens of
minutes to a veral? hours after some chromospheric flares
proceeding the geomagnetic storm. These protons freely
penetrate into polar areas approximately alongtoermer's
trajectories and produce above:them almost uniform coin ?
tillation of greet extent. Since hard protons penetrate
below thee 100 km level the ionization which they
create is
accompanied by an intensive aboorption of radiowavestand
tha radiation contains intenuive molecular bands which mask
the hydrogen emission. Polar areas are very convenient or
observing hard solar protons. Ground observation and those
With the help of rockets and cputniks, even at short dist?
\ .
ances from the Sarth. can provide extremely valuable data.'
Cinco it is sometime-a conjectured that hard solar protons
. reach :the-Barth along magnetic lines ,of force which 'origin?
ate in the .'un some insignificant variations may be expected
in latitudinal boundaries .of lights due to different con_
.
figuration of the cumulative magnetic,field and corpuscular
fluxes above the northern and. southern ,polar areas.
Ordinary aurora are known to have the 'form of a
halo around the gepmagn tie poles at an average distance
of abut 230. DuringgooMagnotic'storms zones of aurores
extend and their center shifts toward low :latitudes. A
similar Shift of a smaller extent is ,observed at evening
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hourssreachinc it peak at local .idnight,whereas toward
merzling thl motion i3 ravened. Radiance is highly non
uniform with regard to latitude and longitude. The low-
-intensity diffuse glow usually spreads over vast nurfaces,
where sometimes additional sharply-Outlined formati.ons.
appear.such as arcatatrips.loopstspots,rays. The more
concentrated.contrasted and less extended are these format-
ions, the. le stable they. aro. The Sharply-outlined format-
ions contain the smaller part of the auroral rdiation, the
Crater part or which occurs in vast .diffuse, fields
45
poorly visible:because of the low.contrastsnsitivity-cf
the human eye at low illumination [4. 35] .
. :We wish to lay 'special emPhasis on the above -
mentioned .facto for they ,.ire of great importance for
general energetics of aurora because during recent years
paramount importancehas been attached only to visual and
c ' ?
photographis dbeervations of the Most intensive.ahortly
'defined areas ofaurores.
,
?
-Ray-like .formations are especially interesting
among the sharply-outlined forms.- They. appear from arcs
? and strips whieh'become .thinner and break up into separate;
. elqments- Separate. little rays have different decrees .
of focusing. Some- of-them. are only hundreds. of meters in .
diameter. Zuch separate rays are very short-lived form- .
at ions ?which exist .less.than. one tenth of a second. he
'thesethin rays aro?especially sharply focused. they ?
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usually flare at certain pointa forming sheaves. (accumolat?
.
ion Of thin rays) along some atruisht or curved lines the
majority of which coinsido with the geomagnetic parallel*
When such rays are focused poorly- their sheaves merge into
oneoractically non?scintillating column.. Sheaves of
sharply ? outlined rays. or solid columns are drifting along.
.tho geomagnetic parallel at colossal velocity both in the
western and the' eastern directions.
We observe drifts at 100 km height which sometimes
reached a. velocity of several km, 60071 (4.] Some authors
. however, noted.. velocities reaching 20 km sec-1 [38]. The
formations extending along. the parallel sometimes have a
wavy structure and form loops and-little horseshoes. -The
latter, as a rule,Tare turned with their convex side eastward.
When we ace ascafilmo moVing at .a high speed
Vortical movements of radiant formations are observed E4,
37] ?
The pattern on aurores sometimes consists of numerous and
.diverse structural details and coruscates with very short
periods from fractions of a second to several tens of seconds.
Calm forms are usual at evening and morning houreperuptive
for ? at 'midnight.,. Some past observations of the minimums -
of solar activity showed that calm forms predominate at such
periods.' 1obile,sharply?outlin4 ray?like formations are
sometimes accompanied by the so?called "weather?vane effect"
- [41. As a result of the relative motion of tho,ray of the
,exciting agent and the atmosphere the. front of the ray has
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-16-
colours of low-inertia emissions,and areas behind the
moving ray have colouro of inertial emissions.
It was already shown.in..3tr5mer's classical works
[C5 that,in the sunlit zonetrays appear on the extention
of geomagnetic lines which cross rays in unlit atmosphere,
Thus the ray weakens, as it were,beginning with its lower
boundary, and then dies out, but begins to glow again on the
boundary.. of the night shade. This additional glow can be
explained by fluorescence in solar radiation of ionized
nitrogen molecules which reach very -great heights along geo-
magnetic lines. We macceededlhowever,in discovering a- -
somewhat different phenomenon [4.1 ?It consists in th., fact
that a ray in full darkness at some distance from the lower
boundary almost suddenly decreases its brightness several
times an metimes even more than by one order. Sometimes
rapidly moving sharply intensified clots appear in the ray. -
It appears that such luminiscence details are due to
streama or currents of the as which rich in effectively
excited molecules and flow in tho dissociated area of the
upper atmosphere. This presents an extensive field of
investigation by direct sounding of the upper atmosphere.
. During the development of ray structures the-ab-
sorption of radiowaves in the layer D below these structures
increases drastically. This shows that either harder cor-
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puscIes or X-rays develop at this time (which penetrate into
the lower areas of the atmophere) due to hapder electrons.
Appearing in the area of-lights [it, 33, 591 .
.Durinz.geomaznetis. storms the width of the band
: of polar light be much.greater. amissions or Polar
lights can be detected even visually at a distance of
. .
thousands,sometimcs even several thousand kilometers. from,.
. the most intensive areas. :Violas of hydrogen eMission. are..
more diffusive and uniform . than omission fields without
hydrogen -emission. 2aximum intensity of the .former lies
in more low-latitude areas than maximum intensity' of the
:latter. -However*the fields of the latter . penetrate into
low latitudes .much deeper than those of the former. Thus,
as a'rule, the former are generally framed with the lqtter
on the side of both high andjow latitudes. In sharply -
outlined forms Of aurora, including ray-like ones, no
intensification of hydrogen emission is observed [4,
some investigators.point:out that fields of hydrogen ..
emission even avoid locations or sharply-outlined forms [40].
it must be noted too that beyond the area of maximum
intensity atomic emissions predominate, this fact showing
that dither the corpuscles are more short-range or the
atmoaphere height in the area of maximum intensity becomes
greater due to intensive heating. Aurora and hydrogen
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18 ?
emission.often appaar in usual polar zones even on magnet?
ically calm daya. with high and zero Eindices,including
yea= of minimum solar activity.
During geomagnetic perturbations only the develop?
..ment of intensive emissions over greater Earth's areas -
becomes more probable. Low?intensity visually?observed .
arc?shapod radiances have been recent/ay observed by Barbier
and flooh11,21 et low iat tudes. They result from insigni?
ficant intensification of the red forbidden emission of.,
oxygen 6300 t. Recently ,Trutze 131 has been trying
to find such formations in the Ashkhabad region (Turkmenian
S.?41). He has not found solid arcs, but observed separate
spots in the red and green forbidden emissions of oxygen,
which do not coinside. /ow?latitude red arcs and spots
are a new and-little?known Phenomenon. The sporadic
non?uniformity or. additional ionization of the upper atmo?
sphere should probably be Included in.similar phenomena.
We have dealt,hitherto, maInlY with processes
within the area of the observed rores. It is not less
interesting, however, to investigate higher areas of the
upper atmosphere from which corpuscles Causing lights
penetrate downwards. In ay,1958, we made an attempt, with
the help of the. third Sputnik, to find fluxes of geomagnet?
ic corpuscles s/ightly above the area or aurores 121, 22,23, ?
24.] This attempt was successful. It was for
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the first time that at an altitude of 1,000 ?2OC kin ? :?
. fluxes of olectronu were discovn.od with an enerey or
abou t .10 kev. Liemely, they were e/e ctron s which are the
most . responsible for surores. But they were not 'hard
corpuacies of radiation belts. Their flux excoeded
N f.12 14 -1-2. ? ?1
? pa r C111 sec ? it ,,Nas found. that
though the *direction of most electrons of such fluxes is
nfarly perpendicular to Gezma6netic lines,' the, directiun of
some of them a) incidca with these lines. Similar fluxes
were later observed by oth,t.:r scientists [4/ , 42, 43, 44] ?
It iz especially intereating that OfErien and Latxchlin,
havina found sucll intensive flu'Aes at an altitude of 1000 ki
did not find them in th-: equatorial plane at a aiztance of
several terrestrial radii [44]? Accordin& to is:round
observaLions, carpusclus which are responsible for aurora,
az we have pointed out many times, have moderate entlr es.
fano? the period of drift of sucb particles around the Earth
is lone as o=pared witb their lifetime, we expected that
they would form only separate fibres around geomacnetic
lines 15,v- .2(?:,] 0 However, *.ut did not admit that such par?
ticles fora) radiative zones.
' It is difficult to interpret\, the drift of rayed
structures as a drift of compact c/ots of corpuelel ea in a
,.? ,
geomagniftie fluid bcaus of theenormous volocity and
different clirections of the drift. This requires rejection
'
;
ill I
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?20?
of the dipole field and assumption that in the equatorial
'.plane at a distance of several terrestrial, radii there are
very complex magnetic fielAs of varziing intensity. Besides,
though aurora around the northern and southern poles are' -
generally more or less simultaneous and: conjugated, the
similarity of their detailed structure:is not yet proved
[45, 46]... :Outwardly separate thin rays :rather resemblo.
some discharge al:Ong geomailletic lines. It In not surpris?
ing that only recently ourora were generally interpreted as
a gas discharge. it was also ouggested that the drift of
electrons and protons in different directions results in-
the development in the exosphz!re of electric fields which
affect- the stracture of aurora [603
Since 1957, at first with the help of Geiger count?
_
era, an accumulation of hard charged particles which formed
stable radiative zones was found in the geomaznetic field
[47, 48] ? Though,in contradistinstion to our experiment,
it was impossible Ito acertain una4biguously the presence
of key electrons with the help of Geiger counters, never?:
theless, the data ibtained with such counters were
interpreted as the result of the
effect. of Xrays
electrons with energie.s of tens of key upon Geiger counters
enclosed in :sputnik. ah.ells? itwac. also a awed that
from
fluxes of such electrons reached 101.1 ? 2012 particles
?2 ?1
cm sec . Later Gringaus, ZurtInoroz and Shklovisky 49
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on the basio of data obtained by means of ion trapsofound
that near the equatorial planetat a distance of several
.radil or the zarthl the ?intensity of electron fluxes vas
about 3 orders' leas than had been expectea. Later this
fact was conf1rm4by O'Brien. Van Allen and Frank [501. At
the saze time Oringausw Kz.;rt,goroz and ;-hklovsky faund sthalI
. electron' fluxes with individual eleetton energis exceoding
200 ev-near the equatorial plane at a distance of' about 10
.B;arth radii. Tho registered flux did not ev.ceed 103 .
. particles cm zoo. The authors thought that they had.
found a new radiation belt. 1:ot so lenc. 4v7o Davis discover-
.
red in tho geomagnetic field an intensive accumulation
of protons with enerzio of 0./ to 4 Zev [5i,) . In the
'end it became evident that .the entire space in the Geomag-
netic field is filled with varicus'eharged particles with
,different energies Confident distinction of separate radi-
ation belts there become:4. conditional. '1natead of the
former "belt' tho terms "inner" and :neuter" zones becolle
more
and more popular for thu.reflact th::t nature of tho
fact more exactly.
?. Radiation belts appear as continuoustnon-diocrete
in longitude accumulations of charged particles trapped by
the geomagnetic fieldpwhose lifetime greatly exceed one
circu/ar drift aroun the Zarth. Accord: to thecio notions,
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- 22 -
particies.with a pitch-angle of about 90? located near the
equatorial plane are the most stable ones. As the angles
decrease, particles undergo deeper oscillationd along the
georiagnetic lines, their lifetime becoming much shorter.
As a result of this,the density of particles 2.1,,Jar the
equatorial plane is much higher than neer polar areas. Then
such conjecture became widely populariSed it was hoped that
aurora are a stago in the deointegration of radiation belts.
The present factual data,however, make such hopes rather
doubtful.
The intensity of the hard particle!: flux in radia-
tion belts near the equatorial plane during the maximum
radiance of intensive aurora,which accompany geomae,netic '
storms, is decreased and is restored only after this aurora
cease to exist [523
Howeverlthe energy content in dadiation belt .
cannot provide for auroral lights even if they take place
at a magnetically - calm period. All this is redoubled
during the existlnce of rey-shapped structurea with a sharp-
ly increa;:id lights density.
We shall cite some exam21es? characterising the
intensity of auroros. han determining the intensity of
aurora we assume that about 3.103 parte of the total
energy of corpuscles having individual energies of about
10-8 erg turn into visible radiation of aurora. On the
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? 5th of November* 15G, in L'ilurztansk,,.at
time, we observd the ourQra for haIf.aa
? index ? being about 1, rthich ho,d th
?
13 hours univetsal
hour, the universal
for:a of a spiral
with numerous tviwts'und diffuse radiance. t,lhich ciwered
.16
an area from -10 ? cm from the =stern bcJrizon to 450 of
the eastern zriith diatence. Th,?;,westward extent of the .
aurora beyond th.e. horizon Is not known. This, aurora pro?
duced illumination of tho :!;1,1rtht Surface which exceeded.
.the inuminatien of the full W,00n, , i.e.. not less than 6.1
?-1 ,
erg cm .sec . Thusgan, energy exceeding' 5.120
()-
erg
.
waa releaaed during. ha1t' an hour.? ,uch aurorae could be
produced by a flux of electrons with an individual energy_
? ?1
of 10 key, exceeding particles eta2 aeo
4:41
the 11th of l'ebruary, after?raidniEht univereial t tale,
one of most spectacular polar lights -in recent. times. were
.obse..ved. The univrsaI index
spread probably over. at least 50
X reachea' 9. ?ha 1i4L4to
A o the 'Larthls curfl,Ice.
The int...,nsity of visible' illucalnat ion on the ..7.:artht - n ?
Surface was not than 1 erg cm-2seo-1. The lichte
continued for several hours. They were oboerY.-.id alloy? America
longer than in 'our country, with an intensity two orders ,
higher than tho ono mentioned aboYes Thus, durina this
event energy reloase in the Larth's atmo43phere only durinj
1 sec .could exceed 104 erg. It means that an electron
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24
flux with an energy of 10 kev on an average could reach
?1
5.1010
particles am72 sec? avon assuming that our
estimrlto is otaggrated and should be decreased by- several
order'a, it is all the 8t1;i9 evident that tho energy content
in .radiation belts le not auffiaient for such i=eriF:e.
energy releases.
O'Brien. Van Allen' Roch and Gartlein found inareaa?
ed. intensity of hari particles abovz:?.,red low?lati?tude .arcs ?
[53] . such discovery, .howevor. cannot .ba considered sas
the proof that ,red arcs are provoked.,by hard particles dumping
from the rs.d'4.4:tiori belt. ? if theze area.% were provoked by
? such particles', then, as. has already bean mentioned, the red ?
emission of a.tomie oxYgen would,no do..zbt, be supplemented-
,other emissions corIespon.ding tO a higher ez.citation ?
,pOtential.. The. pecal?rities of. the irradiation of red
arcs zhetv that it ir.,A?th.rJ result of either the high, tempraturo
of' ionosphere or selective cilemical reactions of ions which
am carried up with the upward current of air. So in both
caoas the swelling of the atzosphore in the red arc area is
postulated. In aadition o thisothe above processes may
induce on electromotive force. A./1 thii: taken seperatiely
?arid in? combination,' mc.ty stimulate clumpino of hard per ticlos
.. frem the radiation belt. It is interesting to note that
i . . .
:a:6g and. Aoch [541 report lower density of electrons wi.thin
I
,
.? ? ? , . ,
? .
, !, ...the rod are area which probably proves that there ionosphere
,.., 0,? . ? , , , ,
1,
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is higher.
The same considerations as affect the inner belts
chow that the new . outermost radiation belt suggested by
EUrt,Zoroz and Shkiovsky cannot be the cause
of aurora either. .This belt is supposed to lie in the zone
of the interaction of interplanetary plasma or solar wind!! ?
and the Larth's geomeRnetic field where the
geomaL,natic
' 'dipole field is seriously distorted [55. 55] . Therefore .
it is far from clear whether the drift of charged particles.
around. the Earth exist and whether they surround the
Earth with. a?,continuous,beit. it cannot be doubt that
the appearance .of energetic particles in this area is
unambiguous eVidence of the interaction of the int erpl a7
netary plasma or "solar wind". with the geomagnetic field.
? But this accumulation of energetic charged ? particles may .
belong not to the' terrestrial, exosphere but to interplanet?
? ary. plasma or lsolar wind". which flovs 'round the geomagne
tic -field, i.e. 'the above accumulation of energetic charged
partici es is net the- Earth' s *radiation belt. All, this can
be determined only by data on the deflections of magneti
fields,which exist there.from the dipole ?geomagnetic field
and by distributions or pitch?anzles of regintered partic?
les. This is, however, a 'subject for future investigati ons.
It would be also especially illustrative to inject artifi?
cially into this area charged corpuscles which are not
present in the natural medium, and Lo observetheir
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.26
lifetime and distribution round the Barth.
The essential role of radiati6n belts ina in aurora
an be rehabilitated by findinz compact clots of corpuscle's .
in the equatorial plane with the help of apparatus of high
time resolution. The analogy
discrete corpuscular fluxes in
,suppoce in 'principle -a similar
plane. Very dense corpuscular
witn the appoarance of '
rayed.aurora allows us to
process'in the equatorial -
clots may remain unobserved
because of the low resolution of the recording apparatus.
. We noticed acmothing of the kind in our above-mentioned
experiment,on the third sputnik at moderate altitudes.
. Further, studies should probably take into consideration
such a possibility.
Presently we have no exhaustive data on all the,
details of aurora and accompanying phenomena. There is no
conclusive theory in this respect either. 7e are not
going to review the relevant modern cenceptions (see,2
for 6:amP1e, [57. 551, ). However.it la beyf)nd doUbt that
aurora is one of the most essential chain in the Interaction
of the geomagnetic field with the interplanetary plasma
.(or "solar wind". ) on the one hand and of the whole
.electroconducting ionized upper
tary- magnetic fields,aa well as
atmosphere with interplane-
with th geoma3netic field
during its own circulation, on the othn. [21] .. The effect
of the direct action of primary solar corpuscles for which
, ?
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only polar areas are open is of little illportance fr(xn the
.energetic point of view. The change of th itneity of
the geomagnetic field in any place of tha circumterreotrial
4 . space is a cumulative effect. Of the interactin complex
current systems of th* surrounding space. It is difficult,
therefore, to expect an exact corrolation, of thc local
energy release of au:mra and. the (lett& which characterise.
the disturbance of the zrazntic field, Chapman [57] aosumes
that the ring current of radiation belts during the geo?
magnetic ?storms can provoke in the equatorial plane lines
with zero value of the gitomac;notic field which; result in
? concentrated formations of aurora. This idea is very attractive
But concentrated fomations develop during aurora at maenetic7
ally calm periods as well. Besides during geo:na,rsnutic storms
the intensity of the particle t/ux in radiation belts during
polar lights becomcrs lower which indicates that storm?time
variati.cna depend not only 04 the drift current in radiation
.belts but on other systems of currents near th Earth as relI.
. :further observations are necessary todraw more coavincing
conclusions.
?Setting asidz .the.less important phenomenon of,
'radiation belte is necessary to make'a speci I stress on
the fact .that huge planetary energy rleases which accompany
some aUrores are sometimes even greater than the energies-
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Which are uouakly tiicL6ht to be roica4,iQd by the a,ccompia--
,
. _
nyin& geomagectic sterms. A satistactory correlation of
these facts is-vry import
nt for complete underst'andior ng
hA) phenomena of aurores and geomagnetic perturbations.
Ziace the Phenomanon of, aurora is asseciated.with
the intrusion of intensive corpuscular fluxes of a consi?
derable energy into. the E,art.1 a a4nosphoretesPeolallY in
thPJ polar areas, it is natu
al to expect
ciat ion of the atmosphere' srolec1es0
corpuscular di?
ay
lead to .a considerable increase Ofithe reaerves of actiVe
.atorts which cause the' for.mation, pf ozone and u2ua emissions
of the upper atmosphere. :rhe heating of the upper atmos?
phore during aurora may incre.a the d.issipati on of
hydrogen
which must of coursQ affect. the.inteasity of hydrox 2
radiation. Besidesvmetastable atoms and molecules may appear
in. the .upper .stmosphere .ander the. action of corpustles0
It must be 'remembered that. fluoresec.!noe of ce.tastable atoms
of prth_heliwct'?has already been found in polar. lights 14.
.,.:Iffoctive excitation of these atoms requires olec.trons ,
with energie.s of about 25 i-ev. Thus fluores ent emission
-of helium is a direct- evidenc,a of the exik.3ter.).ce of a great
nu.mber of- such geoacti.ve elc.ictrons in the upper atmosphere.
All the p oblemo mentioned are still .,insu.fficiontly nder?
stood ad also ? deseve attention....
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1 .D.Barb ler . 544,1950.
?
2.F.Z.Rotloh,,A.14aroviohljourn.%es.Nat.Bur?Ltarld.
3.Yu.L.Truttze,P1. 9,093 952
4.11.1.,grassovsky.P1.0V.I.,
B, 123,193i,
5.V.I.IirassevaieDort to..5ymposium. of 4urorc,l'and Airz/ow,
5 Gnr1 As241bly Of C..?..;.A.G.Iosoow?July 1958.
? Transl.:Pl.p.Sci., I, 57,1959.
5.G.Wirmor.The po/ar AurOra. At the C/urehdon Pre.as..
(Ixford,1955.
7.J.W.halyber/ain.:.'hys1cs of the Aurora .z:.nd
ixadealo Preas.New. York and, Loadon,1951..
8. i?#444.Porsith.. 1794953.
9.B,A.Bagaryatsky.Coli."Spect., SierArophot.and Rad.Invest.
of .Autorao and Uig?it.Airlow" published by Ac.Sci.T.T3aR
No. 2-3$21, 198S..
10.Y.Uakura. Rep./oh.4e1.4.Ja:dan,12,459,1958,
. 21.Yu.I.Galperin.;21.Sp.ci. 10, 18791953?
12.a.ontalbetti.journ.Atm.Terr.Phys.,14,200,1959..
P1.0p.Set., 2, 130,1960s
1441.11?Llhef0VoPlop3p*::41., 10,73,1953.
1.5.J.A.1han aooketA0oriee. 11o.14 159,
Repot
r
30 July 198.
?://e?L
IG(Roo,4t Report Series USA,No.i?154,
July 1953.
17.L.H.Moredith,L.R. ;)EVIS C 1.,..iLlopnA7-,....;.0f3erd. ICY iloc ke t
Series UZA,No.I,159,30 July 195a.:
,
. . :
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2.
18. C....1.1wain.,,!ourn..GeOpilys.., .
im????.?
12.
2(.. V.I. Zrasocvaky cort to L,.:-plqolt,ot of tmtollitou
rockAs and .5allon$, 5 t1,1,,neral Assb1y or C.S.A,G.I.
ccow,JuIj i.1
*Trr7151,,:
219 I. f.-xas o v Iv, e. port , toLymp oolurn f at ell it s, roc s
and -ballona, 13-AusuGt 195E.Trans.Intern.Aa*ron.Union,
Urn
22. I. sacvsky? . 1. Gal per in , .
,rocae dinz3 o f the I:.:oscOw Coszic ay
Conf3rence y 1959,, itc.Zci.U, 3*. 591195C.
? A
23. V. I C; 1raS50V34, I. ;.; A f:liklovsky, Yu Gal
litsky4 E4shnir, G.A.Bordov3y.
Ac .1"4ci .0 3f,',,Xo .5 113,1951 Jp.Sci. ,
77,1962.
. .A.J.1:;assler.Journ.Coc:phys.'::ies. 164, 397,1959.
25 ,L ,:")LIciura..Journ.Coophys.lies. , 55, 40537 11
P.V.3hcheGlov, PI , 10, 215,1933.
25. T.?uIyarchik,
27 ? ',4.V.Jorjio oer.Georiz ? No 5,71411930.
1789,1959.,
? 28. 1.es.
29. G:ivc-AnovoIodny. cl.,10*21,1963.
30. G..Gartlein, G.Sprase.
105; , 1952.
31. Journ. Geophy a 521
32. T .0bayashi .11.akura. :Cp * 3c1. * 5, 59,1951.
33. B?P Sandford.Journ.Ltm.i.err.Phya.,29,/ 52,1' 2.
r
,?,.,A;;;;Ti ? S.A.; .4, ? .:1 1 4".0 .4 4.4
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.11
Cl.) 10,1 Co
v%) ?
K V 'orj.t.o.,;oU. et. ..lewtIrorkIDt.and
aurora and NI,
,1'..)5) ?
.Centhoi t ? s' . ? ,i,235,19,5,2.
nublia ed, b;r c
37. col e 31C ,129 1963.
33. ,1S Potapolra Z.To Bor Col .1.
Opect.o_
L;lectrz.,-ipho t.and A.ati..Lnvoat .of Aurcorri and Night; Airglow
- pub 1/ Waia, d A.?
9.."*L.Vaiborz.::,c11*. "ror and Airalow" d
.11;4;;I,: 9 i7r) 4; 3 935,19-C)2.
40. L.a.-:-.i;v1ashin.Geoura,;.Aenvn.U:,.1;3.liti, 54,1961*
* ?A Ant onova , v o any ? z Ac
.iseefiz .1 No .51755, 19(30
.42.L. A. Ant onoAra. tzv ?Ac ? s geofiz ? ,,i,o.::;;11..437
1951 ?
43. A .13avartko ? '7e41.3hir.rri P.1 oar on ko .tok. put
7 5 ? 1 .
4 . . C Lanahl jou rn ophy s , ? 2237
1902.
45. 11.1741 tviot . P1 .233). 8i4.2,19&1.
? 45, 0 va ory ji'.;?*.173,1952.
2-3, 42 fig (5C; ?
47. Chudakov? of ,
Cosmic :1?:',ay Co
I .19(30.
ranee ? ?Tu13., ';'; 59 ? r.1.11)1 1,..e
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?
48. 41- A . Van, Allen .
Conforonce,c3.'41d
49. 4..17. r V .
:131t. ? put.
#
4.
!7'rocUn Of th. oticovt Conic. Ei ay
d
. ?
, ;L:-?'.; 2.
?
50. . J.C.* 3ri, en , J. 4. V ara on,C,D u.4;121 in , L. A. Prank.
7,152.
51 Kahl ? Acapo . Ca 1 Chap rnan?
Jrn.Gyi. 1952. ?
. f 17:za a ,irno J. inoklb r ? Jciurn-G.a. .
4543,152.
53. 13. 1:',r len , J A1.1 on 2 C 1;) ? ? Cart a in..
joUrn.. Geo .11# 27 fd(30.
5,.1. .11.1x .1!, 'JO urn Ile .liat .11= .;'t and ? ,
D55,129,195-1..
55. P?J?Col eman. Tho reL;ion of geoza6notio field.
.13 inter.Astrc.)azzu.tie..3. Con:t.,7,..$ Varna, Bulcaria p.1952..
55. J ?He ..)pner N . ?;.; ;7;. arc o T . Z man .
Jour r.. C opla.. .no .1,19,53. -
#Okla przi r le an '."2,(11,3,n. t is t ;),.;) . 4,24 1
58. j. Pidd.ing,t on., PI . :??*p. Lei . 90, ,
59. Z.. A . Ln der eon . Jou rn.. Zoe . jz.1 nan , 17 Cupp
237,1R 2.95?
6.
u.V.4..:ha:41beriain
134,401 ,1)r31.
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? ?
? . ?
.7/4A'?4-
TrP 4
it-
ogriz..:?ircm.S
7
112212 1-CECH r
ART12ICIAL L'ALTH ZILILTZ
3" and " CO ;.:..0 :3 5"
- I.21Analt
V.I.Zrassovsky
Institute Of Attospheric Physics
? Of the 11R? Academ,;, of Z;ciences,Loscow.
Th. continue the research of geoactive poriscle begun
in nay' of 1955 by means of the a:hird LoviLt 3putic l'.68 6 2
( 1, 2$ 3 )9 aperfected equipment install ip
? c003 3 . and CO.CL7C3 5 was?wied. These sa '.re
' long-lived geophYsics. stations. :They functl oneci in ?
7 490 at .altitudes ranging from 203 to 1 (3 km '(4). ach
? ?????
?
Of these satellites .carried two? chareed re:at; traps,' .
/0 rt -77?4i3
five ,r4t0t Ole crox1.....inc419P.:,4ySrP with fluorescent screen- and a '
G-L; counter shielded with lead and intend for reistering
most hard particles. The traps and the inicc-Itors were located
outside the satellite and had different aperture and _utual
orientation. 1:1:0 orientation of the traps tn...1 .) --ators
is shown in 21z.l. The arrow indicates the axis Llir:_y,;a of
the viewing opertures of the traps and the indica,
The charged particle traps recistered th- total
current of ion fluxes and electron fluxes o' c-nerLici.. aixceedinz
? certain thresholds. The principle or olw.:rati uf the
traps is illustrated in Fig.2. Y.etal gr4:dz are coul)led to
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body 1.. .A potential of 40 V preventing thermal electrons of
the ionoaphere from penetration into the ,trap was applied
to.grid.3. Variable voltage which retarded positive ions
was fed to grid .4. As. ,a result of that,admission of ions
of eueraios bo1ow.0.15 ? 3.0 ? 6C 7- 11 ;:tV is'stopped 'by
-turna. Within a part. of the.time Spent the gitid was deener?
gized and,its potential relative to the body equaled ZOTO?
.The variable voltage mentioned above does not influence
practically the electron fluxes under research. in collector
5 waa placed in an intensive field of permanent macnet G.
The magnetic field.sharply reduced the sensitivity of the
traps for electrons of energies below 5 keV. This magnetic-
field similarly influences ions of the same Larmor radius
which approximately corresponds to the enery of 30 eV for
. ions of atomic oxygen _ O. . Besides, the magnetic field,
which was almost parallel to the surface of the rint3.c011ector,
restricted leakage of secondary electrons and photoelectrons -
.of low energies from the latter which arose as a result
of irradiation of the collector by the sunlight and corpuscles.
hen the trap was directed to the Sun, its current value from
the silvercovered collector with the area of 43 cm2 reacAed
approximately
10-11 A. it means that the. Configurati on of the
magnetic ? field applied ;reduces the photocurrent from the .
collector to the body by not less than 4 orders ,of maEnitUde.
On the other band, the photocurrent values r'fiistered were
.COU80q by photoelectrons of comparatively. high energy.Their
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? 3 ?
analysis will permit tz; obtain inforzation of the u14,raViolet
radiation of the Sun.
? %'he effective solid angle of the trap for ions and
electrons of high onerey equaled approximately 1 steradina.7ith
respect to particles novino at an ancle of 3,,,o relative to
the axis of the trap its sensitivity is only twice ac low as
for aqial ones. This s.zoothed or the effect of rotation
o: the satellite when anisotroiic fluxes of corpuclos were '
registered. The scale of the tTap current amplifier permitted
--
to recister positive Isotropic currents inside a so/id angle
of' about 1 steradian within the limits of 3.1O to 5.106
ion cm-2 sec ster, and auisotropic currents with a
?1
narrow disk ? shaped.distribution within the limits of 3.106
? 1
to 5.107 ion crii sec1 eter? (provided their ?speed is high
enough to penetrate the macnetic field or the trap). In
another trap, in contract to the one described above.grid 4
was connected to the body, whereas a positivQ potential of
24 V was fed to arid 3, ?preventing froz penetration into
the trap-the ions of energies below 24 e7 (with the uncertain?
,
ty equal to the sum of the satellite's body potent :d1 relative
to undisturbed environment and the contact potential differ?
ence between the body and the grid 3). At the moving
satellite the eery of relative motion of ionospheric ionr1
was under 15 eV, therefore ordinary, thermal ions of the.
upper atmosphere were not regitcred. In tiA.a. case the amplifier
scale permittei to register positive currents of 3.105 to
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?c IV 01
E rcror
4 -
Stet?-t
3.108 ion cm sec V for the isotropic flux and from
to 3.109 m ion c see1 for the anisotropic one.
The electron indicator, whose dies...ram iu given in
Pig.3 consisted of thin fluorescent screen 5 put on glass
plate 6 and covered with aluminium n)ii sheet 4. Yletalli'zed
screens 5 with foils of certain Indicators were fed with
a positive voltage relative to the body accelerating electrons
and periodically varying in steps. esides that, a potential
of - 40 V relative to the body was applied to grid 3 placed
after grid 2 connected to the body to bar the way of thermal
electrons of the ionosphere to the screen. Fluorescence of
the screen was registered by photomultiplier 7 whose signal
was amplified and applied to the radiotelemetering system
with a memory reginter. The amplifiers were equipped with fine
and coarse channels which provided for measuring the intensity
within the limits over 3 orders of magnitude.
The indcators responded both to electrons and
protons whose ranges exceeded the thickness of the aluminium
foil sheet. A small part of soft corpuscles was registered due
to accidentally thinned portions of the fbil. in addition,
electrons which did not penetrate the lb lie influenced the
fluorescent screens by Xray bremestrahlung.
Additional accelerating voltage increased penetrat-
ing ability of electrons. As a result,our indicators were
able to register electrons of small initial energies. For
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? 5 ?
instance, the indicator with a foil of 0.4 mg cm2 at an
.additional acceleration of 11 kV was able to register electrons
of energies above 40 e7 (this threshold ip determined by the
potential at zrid 3 mentioned above).
Zlectrons of energies from 40 eV to7 keV d)uld
be registered .in ease the isotropic flux exceeded respectively .
2.108 and 2.106 m
particle c-2 sec ser iv? the
?1
? ? . ?I -
energy flux. beginning from 2./0 erg cm2 se1 c ster,
for energy? keV and about an order of macnitude as low
for 40 eV and 7.keV4 .However at
of 6 kV the Sensitivity for such
- than 2 orders of Agnetude. With
an accelerating voltage
electrons decreased by more
an increase of initial.--
energy of electrons the ratio of signals at aooelerating
voltages of II and 6 kV decreased. At initial energies of
electrons exceeding 20 keV the sensitivity of the indicator
described was comparable at all additional voltages. The
less the initial energy of electrons was, the deeper the
modulation of signals was 'which permitted to estimete this
energy. At satellite C0.CY03 5 the same voltages as being
applied to the ion trap wore ueed for additional acceleration
of electrons. At satellite
the indicators were 2.5 times lower'
the trap. At odr satellites use was
'72
1.4 ? 10-3 cm .of fluorescent
3 the v8'Itagee fed to
than those applied to
made of indicators with
substance Sr3(PO4)2 rEuI
screened with aluminium foils of 0.4 10-3 and O.8.10-3 and
?
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\I a cm2. Only Only at satellite ccYznos 5 together with the
roil of 1.1 . 10 ) a cm use was made of fluorescent screen
5.t ? 10-3 g cm-2 thick (made of &IS ). The comparison
of 4ata of the indicators with the foils of different thiec-
ness is an additional source of information about the -range
of particles and, consequently, about theirene,;.,..ey., Signals
from. electrons and protons With ranges exceeding considerably
the foil thickness were not modutt:Ited ,when an accelerating ?
voltage wa8'appllqd.Tbis comparison permitted to distinguish'
these signals. from signals of lower energy e1octronE..4.
'Due to the spatial cnisotropy of charged .particle' ,
fluxes in the geomajietic field :th rotation ofi a satellite
also causes a typical modulation Iof a signal registered.
41ectrons of approximately 1 =eV .and ,of a higher
energy penetrate through the Walls- of the indicator body.
Therefore the aperture of the indicators which for ,electrons
of small energy 'was' equal ,to cv 1/12 steradian inoreased.'ffar -
?
hard particles and aiyost reached a hemi-sphe.re. During* the.
? . .
? \
rotation of the satellite the modulation of siwneas due to the,' -
/
anisotropy of such an electron flux decreased .and vceased to
?
be deep. This circumstance allows to identify such corpuscles.
Pig.4 represents a pattern_ of the' signal record made
y means of one of the' indicators of satellite GO2ZOS 5.,
The record reveals two types or modu.lati. on. One of thee is
due to the stepped variat on of the accelerating voltage and
the other-4s caused by the satellite rotation in s.nisotropic
field of electrons.
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-C-41-c:14/
Is* II? 41Jcii
t
6.1u 1-1 4y,.,
Fig.5 represents signal records of the other
? indicators instal/ed is satellite C05141,D3 3.
? The Axes of these two indicators and the satellite
axis of rotation were mutually perpendicular. The axis of
rotation lied .J.n a plane perpendicular to the magnetic line
of force (see Fig.3). The data records or thss indicators
have a phase shift equal to 90? and 2 maxima within one
period of the sdtellite rotation. They indicate the intensity
dietribution according to the value of the pitch angle and
achieve their maximum when the pitch angle is equal to 900.
The signals shown in Pic,. 5 were produced by very .
hard electrons of energies amounting to hundreds of ZeV.
The experiments carried out testify to the fact that
by means of fluorescent screens and aocelemating voltages
electrons an bo -analysed -within a rather wide range of energy.
If a modulating voltage is applied additionally to grid 3 of
the indicator (3ee Fig.3) then we shall have an instrument '
registering electrons of any energies beginning ,from thermal
ones.
131ectron indicators with flubrescent screens are of
little sensitivity of tba X?ray bremastrahlung arising
at the
expense of very fact electrons absorbed either in the satellite
body or in the:lower lying -atmosphere. This is due to the '
fact that the fluorescent screen are rather thin.
In time thin aluminium foils are subject to meteoritic
erosion. Owing. to this fact they become porous and more
transparent.
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A1(10,0
1' ro')S 7 r.;
When la the p.17;_,coml of th*)' catilite rotation the
?vietang aperturos-ol the inaicators are dixeCted to 'the Sun9'
a ,klignal.app'zIara vhich. indioatt- exposure or th .ot photomul- .
tipliera. Irifc'ratir pertaininz.t0 t1 tellite orientation
'roiati otho Sun obtainod additionally by s:ecial indicato a
-
permits to iotingUith sach phcno:aeaa and exclude them fro:
analynis of oiznals received from corpasclez. ,c,;hortly after
1aunchin8 the catellite* foils 0.4. and 0.6 Inz cm - thick were
found. to hav crecu their transperence by more than an order
of rnnitudo c copret t10 rcaulto or the, testa carriba out
berore the launchin. iLit5.my have. bei cacised by pieTcinz
:action of mateoritic dust-suspended. i tao ato*here at
altitudea- or 80 to 2CO. 'km or b deforx,I4tt on of' the foils when
th ca i1t enfte,,1tl vacuum. Roweverta rward 2 9 durih
tha flight .i. the vacuum th increaouioT the erosin of theat:
fuil was not recci,Al2:(,,d, oi1 1.1 mg.cm72 thick did,
not revoal any"mark.d aignc; of erocion 'fit all.
671 ,?001,41.1 To facilitatc the compariaen of
'
th data on the -
eoft corpuBalt2a obtained by..zeana, of tflit=nS. 3 and.'
C1)37.10Z: $ witi, t1),. data of radiation belts rceivod before with
the hel. of G-2 muntern. for Our catellitaci we also used guch,
a counter of design ilocribei 1;(%low.
- A. standard ha,ogen G-M_counter cTC-5 ailielded with
_304 g Pb vas inntallA iuide. th o zdte1lit,1.The
? olementa'of ths. construction created a complicated additional-
'shieldinz the minic4m. .Valua of whickl is about 0.8 g cn:1!?, Al
'
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- 9 -
in the solid angle of about 2?11 Eter and approximately up
to 25 g cm-2 from the other directions.
2rom the counter the pulses were applied to the chain
?.consisting of 12 triggers with totalizers whose readings were
? transmitted to the radio-teldmetring system. The effectiveness
of the counter for y -radiation of Co60 (1'.17 and 1.33 mev)
-
reached 'approximately 2.102 counts/quantum and for electrons
of 1 meV about 8.6.1e6 counts per electron cm2. The area
of the countor was equal to 4.3 cm2. With such a schielding
the counter practically does not :respond to electrons whose '
? energy ia under 400 keV. At higher energies the Wynter regist-
ers X-ray bremastrahlung with low effectiveness. An electron
flux of I meV which develops a countini rate or 100-counts/sec
- - ,
1.13 equal to 2.3.107 particle cm2 sec1 41 4lecurons whose
?energy exceods_10 meV an. protons over 50 moV pelletrAted
?.
or..sr brieM s, r
into the counter. The high counting rate (approximately 103
sountaisec) over equatorial ret,ins may have been caused Mainly
by protons.whose energy exceeded 50 meV. Increase of intensity
in high latitudes was caused at loast partially by 'the latitud-
' inal effect of cosmic rays. This incrvaso sone times might be
also connected either with solar cosmic rays or with X-ray
?bremastrahlung from rather hard electrons. However, the inter-
? pretation of the counter's records is not quite of a siniLle
meaning. ?
In the course of the research the values of different
voltages feeding th equipmentophysical conditiJno at the
? satellite, current-3 of oelar batteries etc., wire periodically
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?10 ?
checked. In flight the electron indicators with fluorescent
screens were periodically calibrated by means of a beam of
,electrons from tritium targets. The beaM of electrons
in padded by aluminium foil. During the calibration
,1,11344,110q electrons were accelerated by an .additional vol
rlAti4T
?
wa3
these -
age of 11 a
applied to the _circuit between the target and the foil. The
analysis of this information showed stability of the equipment
used. This-stability was specially ensured by the automatic
temperature control inside the satellite.
The subsequent roportspontain preliminary data of
the information processed. The information about the satellites
orientation relative to the 3un and the geomagnetic field are
still in the process of computation. The 'information about'
the atmospheric retardation of identical satellites 00=0S 3
and. COSMOS 5 presebts valuable data of the upper atmosphere
.density it the regions of their ? Perigees.
?
1 .
? 1.
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.1: Or
IC.: 11 3
-------------
-entation of ViewinE Ap?rtures of Traps and iud1catrs
in Satelliten CO:; 3 and OO=S 5.
2. Charged Particle Trap :chem
1).Trap body
2) Metal grid c coupled to body
3) Grid fed with voltage of - 40 I
4) Grid fed, with variable voltage +0.15
5) .Ring collector.
6) Permanent magnet
3. Indicator of 'Sle t.rone Sc e
? 1) Indicator body
2) r.etal grid coupled to body
3) Grid tad, wIth volti,,ge of. 40' V
? 4) Aluminium foil 0 or 12.1:mg Cm- (
5).Fluoreacen't ;screen
CO alas? plate covered witn tiuor.
? 7) Photomultiplier
4. On Zzample of oiEnala Re a
of ,Indicator In$taj.1eJ
Screen 3r3 (PO4)2
.roil 0.4 . mg cm
Record shows. trio type
,
r
tro
iAlit,c ?in 1 .
to zx Ixtepped variation of aceli?po.
reaults from rotation. of 11.4.
,of radiation.
?r1)
V.?
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\et
Record of Sinal8 Received in Sa unite COSIOS 3 by means
Of Two Indicators Vihose Axes Are nutually Perpendicular
One of records is'preoented by continuoua linelthe other
by hatched line. Second indicator ha a somewhat lower
? sensitivity. In present case axis of satellite ,rotation
- ,
was perpeadicular to axes of indicators and meoletic line
of force.
6. Mutual Orientation or Indicators.Axis of natellite Rotation
and Direction of Yagnetic Field Vector B for thu Case
Shown in Figure 5.
LI is the vector of the kinet a moment of satellite
rotation;
ei and e 2 are -ang ea of indicators axes with magnetic
line of force.
Reference
1..V.I.Kra8sovsky. G.A.Bordovsky, G.Y.Zakharov,
Ye.M.Svetlitsky. Detection of Corpuscles by Yeana pf Third
.Artificial Earth's Satellite. Isk.S`put.ZemlitAc. Sci.USSR,
.17 2, pp. 59-80, 1958.
2. V.I.arassovoky,I4.SbklovekyOu.I.Galperin,Ye.M.Svetlitsky.
Detection of Electrons of about 10 keV in Upper Atmosphere
by Uesns of'Third Artificial .Satellite. Doklady Ac.Sci.U5SRv-
V01.127,110 1 p.7801959.
3. 1.I.Krassovsky?I.E.OhkloVaky, Ye.M.Cvetlitaky,
,Y11.M.1ushnir, G.A.3ordovsky. Detection of Electrons of about
10 keV in Upper Atmosphere. ,Isk.Sput.Zetli. Aa.Sti.U&SR,N GO
pp. 113-126.1981. ..
4. c0zP4a. ? Information DulletinoN0.I2, pp.51-53,1982.
,
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Fluorescent
indicator
Foil: Al
-
0.4 mg.cm2
Screen:
Sr3 (F04 )2 [Eul
, _2
1.4 mg.cm
Fluorescent
indicator
Foil: Al
0.6 mg.cm-2
Screen:
Sr3 (PO4 )2 [Eu)
_2
1.4 mg.cm
r--1
Fluorescent
. indicator
Foil: Al
0.4 mg.em-2
Screen:
Sr3 (PO4 )2 lEu)
2
1.4
Fluorescent
indicator indicator
Foil: Al
1.1 mg-0m-2
Screen:
Zn*gl
5 mg.cm -2
Ion trap
Grid
potential
+ 24 v
Paper I. Fig.1
Fluorescent
indicator'
Foil: Al
0.4 mg.cm-2
Screen:
r3(F04 )2 [1
1.4 mg.cm
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velocity
of
corpuscules
2 3i 412
LI to electrometer
tube grid
N6
,l. Aluminium sheath
2. Grids with zero potential
3. Grid with potential - 40 v
4. Grid with modulating high voltage V
which is retarding for ions.
5. Ring collector
6. Magnet system
Paper, I. Fig.?
-
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velocity
to
corpuscules
to
amplifier
V - modulating high acceleration voltage changing
in stepwise fashion
1. Aluminium sheath
2. Grids with zero potential
3. Grid with potential - 40 v
4. Aluminium foil
5. Fluorescent screen
6. Glasp disc carrying the screen
7. Fnotomultiplier tube
FLUORESCENT INDICATOR. SCHEMATIC DIAGRAM
(
Paper 'I. Fig.3
?
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8.1
???? :::,...~s???????ss s
0 tar ????,,,,.???? ? ?? ??? No.
?
16 24 32 40 48 56 64 72 80 88 96 104 112 120 128 136 144 152 160
t (see)
???*.
V (kV)
10
0.15
0
11
Paper I. Fig.4
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t, sec
96 88 80 72 64 56 48 40 32 24 16 8
Paper I. Fig.5
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a{:4, ? ,4 .
Paper I. Pig. 6
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Y ?
STAT
UPna AT=OH'tIliS RE5aARCH BY USING.
? ARTInCIAL i;ARTH SO3LLITS3
COSLIOS 3 and COSMOS 5
2. Soft Corpuscular Radiation
By V.I.Krassovsky,Yu.I.Calperin,
N.V.Jorjio, T.M.Mularchik,
A.D.Bolunova.
The fast charges particle traps described in the previous
PO ill:104'z
report V were installed in the artificial Earth satellites
"COSMOS 3" and "COSMOS 5". They made it possible to record
ion fluxes of relatively low energy. Besides,using a ranee
of retarding potentials and account of the effect of the
.trap magnetic field permit to estimate the energy of the
predominant part of ions. The obtained information pertain?
ing to the trap currents indicates that fluxes of positive
ions with energies far in excess of the thermal energy
are discovered in the upper atmosphere*
The characteristic feature of these ion fluxes is that
,they are recorded predominantly from one particular direction,
? . - ..
i.e. their velocity vector distribution is sharply stretched'
to one side in'the coordinate cistern linked with the
satellite. At the same time, the ion 'flux moving from the
opposite direction is either essentially weaker or even
lower than the trap sensitivity threshold. The prefered
velocity direction of. such ions is approximately perpen?
ftflJ.....
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11=MP
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2
,dicular to Ltamanetie force? ligeg.
The orientation analysis of. the COSMoS 3 and
C0UO3.5. satellites has not been yet completed; nevertheless,
it is already now obvious that the direction from which the
above-mentioned ion fluxes are recorded,does not alPPYA
coincide with the satellite ve/ocity vector and is sometimes
at a considerable angle from the latter. When the trap with
switched-on stepped retarding voltage was oriented by the
velocity vector the ion signal showed no sighs of increase,
while at the_eaMe time the energy of the relative motion of the
ionospheric Molecular ions might increase up to .15 ev (in the'
*stem of coordinates coupled with the satellite and with
due allowance for possible contact potential difference,
between the grid and the vehicle skin and for the potential
of the skin relative to the plasma).
This vividly manifests
that the energy of the particles recorded is of the order of
dozen of ev.
?
The absence of simultaneous signals on the fluorescent -
-screen indicator shielded with aluminium foil and facing the
same direction shows that the range of the ions does not
exceed 0.4 mg cm-2 and, consequently,their ?energy (in case
of protons) is not over 230 kov. The cumulative data obtained
bg using the ion traps permit to come to the conclusion that
the .ion energy apparently may_be estimtel. ............................
tens or ev and only sometimes for some part of the corpuscles
attains to several key. The ion flux usually reached.
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-2
approximately 108 ions cm sec stored-1 with the
maximum recodded values being of the order of 109 ions
-2 -2 -1
cm sec stored (in case of the ion flux which is
isotropic within the solid angle of 1 steradian).
It is rather intereating that occasionally at the same
time with registration of the positive ion signal on the trap,
the fluorescent-screen indicator shielded with aluminium
-
foil of 0.4 mg cm2, records the flux of soft electrons from
the opposite direot,iop.with the energy not exceeding 5 key.
'The fact that the trap falls to record such electrons after it
turns through-180o due to the satellite rotation, also
indicates that their energy is considerably less than 5 key.
If we assume that the energy of the above-mentioned electrons
.does not exceed approximately. 3 kev,then their flux agrees
by the Order of magnitude with the simultaneous ion flux.
The_movomept,of electrons and ions in the opposite directions
possibly .indicates that a certain eleOri-4,AAL.:10,14,,14
able in the ionosphere.
It is characteristic that if such a flux was recorded
during one satellite revolu/ion,it was usually. observed
..during subsequent revolutions at well within:the same range
of latitudes, i.e. at the points ofoorbit specified by the
'same local solar-Iime. In several cases a more or less
sharply outlined region of the ion flux over the equ'ator
maintained for at. leapt 9 hours Oee
The orbitral plans .of the satellite gradually turns with
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4
respect to the Earth,so that the moments
certain geographical region are shifted
in the local solar time. This will make
perform an approximate evaluation of the
described ion fluxes,depending on the loc
the ion fluxes possessing the energy far
thermal energy can appear 14any local tim
it paeses over a
for earlier hours
it possible to
distribution of the
al time. Apparently,
in'excess of the
o.
The above-mentioned ion fluxes were recorded only. at
low altitudes froth 2O0 to 600 km in the F-regien of the?
,M4 441Y ? 0,,V,Gl't00.1
ionosphere. Positive ions, as a rule,, were recorded at a
given satellite revolution for 3 to 15 minutes, i.e. within.a
? range of thousands of kilometres. It' is quite possible that
the observed ion fluxes with the energies appreciably exceed-
ing the thermal energy,pertain to the system of ionospheric
?
S and L currents. On switching off the stepped positive
which
voltage/Nitk generated the retarding potentials, one of the
? traps recorded the ionospheric ions penetrating through its,
magnetic field. This resulted in a strong dependence of the
signal intensity on the trap orientation with respect to the
satellite velocity vector even at great heights.
E'445..0 7'00
The fluorescent-sereen electron indicators with a
variable accelerating potential could record the electrons
in a rather broad energy range beginning from 40 ev. Besides,
such an indicator can record the ions whose range exceed.
the foil thicknesa.
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a
? 5 ?
Let us first consider the results pertainingeto
low-ener eleeteerepee (not exceeding 5 to 7 key) and medium -
am???????*??????/..0.0,..... ?????????66.2.NriAi&aiel,MaWaY,.;Alra?
energy electrons (i.e.of order of 7 to 50 kelt). The. signal
??? Se1 A 0 atl, r>le 71t,.'s+40.9.411,.4."1* Ma,
generated by such electrons was appreciably modulated by the
accelerating,voltage, and the lew7energy electrons were recorded
practically bnly by the indicator shielded with foil 0.4 mg cm-2.
Al at the maximum accelerating' voltage of 11 kV while the
medium-energy ,electrons were,recorded,even at lower accelerat-
ing voltages. The electrons with energieeebelow 5 key are
4
recorded rather often, but eporadically. Their 4ilergy flux .
- -1-
sometimes reaches 0.1 - 1 erg ? cm2- -1 sec steradian(assuming
the electron energy is '5 key or l'kev,renpectively). At
? '-
typical values the flux is approximately 0.03 erg c2m see-1
steradian-1
if the energy equals 5 key. The variation of
such electron fluxes due to height ate well as their anisotropy in
the magnetic field greatly differs from similar characteristics
of other types of corpuscular radiation available in the
atmosphere. Both these interconnected characteristics are
highly variable, with the fluxes of such_pleetrona_being nearly
isotropic on the average and their intepAkey is slightly
? al.Z.44 4" 4" Z +44 - ? ? rar.:: 41.0. -A
dependent on height. The signal generated by the electrons .
4.????"?????1,60,141."*.3,.......41,11.14114o 1,144,4?......verN??61,}.? g
?
?
pothsessing energies lower than 5 key appear at all the latitudes
1.4 a 6 ? "4'4 4,4*?an. rr.62,e31?1 .1/ t????? ir ? Ow" 0 a ? I, 0'.....1,401..1 ? 0.1..V.1.4. ? a a ? ??? ? ? ??
and even over the equator. The characteristic feature of these
.eree.,"....1?W?-9.4.4,????.41Y,44:044,464-4,4T?14?401,14????!11...ar,,,
-at ?61, 6,4 V ???1?1,,,. ?141'7;.:',4,1-4.7
electrons is that they are recorded mainly in theilluminated
L.. ? ?.? .41.946?17?-rizolz?????.,.0.-rt....,44....,,,,,r,,..., AotrA A V' Irry Ar, .1.+10,;-.."4&7
region of the atmosphere. Their intensity on the 'night portion
????????44.444??????????????????comminuanagaliaro*W?2.1?4.14..~.4.4.4
of the satellite orbit is, as a rule, considerably lower than
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7 Declassified in Part - Sanitized Copy Approved for Release 2012/12/13: CIA-RDP80T00246A022400050001-7
rcec
(r. irIk'oet 3
rier
4cc4rciJ
/3)- pi/7/6kt
6
.0
that on the day portion of the orbit. Often this corpucAes case
disappear at all several minutes after the satellite enters
the region of the Earth's shadow.
This information .was obtained mainly by the use of
memory data-storage facility of the satellite when the satelli-
te - borne radio-transmitter used to transmit the'telemet-
rical information was switched off and only the low-power
transmitter "Mayiak" was in operation. The -nature of the
signals detected remained unchanged when the more powerful
transmitter was switched on and off. This Permits to assume
that the electrons recorded were not merely the ordinary
thermal lectrons of the ionosphere accelerated in the variable
fields of the satellite-borne transmitting antenes. It can
not be excluded that the satellite movinc in the illuminated
portion of its orbit also records the photo-electrons origin-
ating either in the illuminated region of the ionosphere or
emitted from the "Mayiak" transmitter antenna surface which
is ithin the field or View, of the fluorescent-screen indi-
cator. Howeverlsuch an explanation is not valid for the night
portion of the orbit.
The medium-energy electrons (approximately 7 to 50 keV:
appear mainly at,high geomagnetic latitudes and at high alti-'
re"1,1"ikewe.43.1.? tid, .?.!.Urs.....4.0.44. ?
tudes. Their intensity dependence on latitudes is more defi-
nite than that of low energy electrons,and at altitudes below
1000 km they appear only from time to time. No medium-energy
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electrons are recorded at altitudes below 700 km in the
South-Atlantic magnetic anomaly. Howevertin some cases
such corpuscles were reCorded at low and middle latitudea
at approximately 1000 km altitude 'where their flux amount-.
-2 -1 -1
ed to some 105 electrons cm aec steradian assum-
ing the electron energy equals 40 key. As a ru/e,the
anisotropy of such electron fluxes is more distinct as
compared to that of low-energy electrons. in addition to
the above mentioned distributions of the electron. velocity
vectors typical for the corp ales trapped by the geomag-
netic field,many cases were recorded when the shape of the
anatropic distribution of the velocity vectors was an
eevidence of the invasion of considerable electron fraction
Into the dense atmoophcre. This phenomenon first detected
in the course of upper atmosphere research by using the
artificial ,,:arth satellite "Sputnik-III" in 1958 /2,3,4 /
and then confirmed by O'Brien /5,6 and 7/ using tha data
obtained from satellite-"Injun-i" in 195/,may contribute
to the energy-balance and ionization of the upper atmos-
ehere /3,4/.:
Besides the above-mentioned fluxes of.electrons whose
signal was to a considerable extent modulated by the variabb'
accelerating voltage, the fluorescent-screen indicators
recorded the particles possessing higher energies. Their
A.a.a bft14 r.mo t A,t4 OW,444,..,/,,445,444,1Mtt
signal was subject to modulation merely due to the satellite
?
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rotation.The distinct anisotropy of these particles with the
maximum intensity at the pitch-angles equal to 900, and stabi?-
lity of their intenaity indicate that the particles have been
trapped by the geomagnetic field. The traps recorded negative
currents simultaneously and in phase with the signal. variations
of these particles displayed on the indicators. This leads to
the assumption that the fluorescent-screen indicator signals
which are not modulated by the stepped accelerating voltage,
...were generated by the electrons Whose energies range from
approximately 50 key up to several hundreds of.kevr but not
by protons with energies in excess of 200 11* .500 key which
can also penetrate through the aluminium foils. Now this
conclusion will be considered in detail.
The signal ratio of the indicator and the trap at
the .pitchangle equal to 900 as calculated frop the oalib-
ration data and their geometria tactors,differs by not more.
than 40 per cent from the.indicator-to-trap'signal ratio measur-
ed in the South Atlantic geomagnetic anomaly.? Now let us
'assume that the electron flux with energies exceeding. 50 kev
.(lower energies are impossible since no modulation by the .
accelerating voltage takes place and the sensitivity of the
fluoreacent-screen indicator with Dela. 0,4 mg CmAl.is
? higher than the trap sensitivity) is added 'with the flux of
protons vith-energies.exceeding 200 .500 'key whose signal
displayed on the indicator isYcommensurable?with.the, signal,
produced by the electrons of over. 50 key energy or even exceeds
. . -
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?
the letter .neneraYLJ. ia ovious that the inc]icator
:igrd1:;.klcud ineren:-ye while trt.7* neatiy,a current of
the tp'ad reoorng_the alg,Jbraic sum of ,ilectrou and ion,
crlr.eats will on the coi.rary, decreaae,.. Conequestly,their
.1/. to a considerable extent incroazle and. will differ
from tne rez:Jults4 obtain-3;d in the Sov4th AtiafAicetic
onaly. It should be also taken into account ha the
o=t?screen indicator sensitivity to the protons penetratin
threll the foil, is rather high, i.e. the energy release par
cno preton with the energy over 2CJO key in the fluorescent
7_1creen and ita light output psllx per uni.t energ:" greatly
,cee.ei& the :.1,x.i7?.ar values obtained per on.t electron with the
eaer:: in e.;:oess of 50 key. Threfore, a .:a1:;1igible (as
compured with the electron flux) faux or possessing
the ,P:.]nctie,,s nent,loned above r the fl-osct other ions)
sinificantly cLan-ed the sgaT'8t,1- of the two.
.pick?u;2s. -llence,at altitudee u:?), to. .700 km in the out Ii
Atlantic mae,netic anemaly,the proton flux is negligible as
.11-3.?
-compared with the flux. of electrons.
, Only approximate energy evaluation of these electrons
aan be made. As has already been stated, their energy exceeds
50 key, while the omnidirectional flux reaches .5. 107 particles
?2 . ?1
cm sac . The deep signal modulatit)m. with tie satellite ?
rotatirz in the anisotropic radiation field snows that the
energy of electrons 'does not exceed 1 mev. This acillelusion
is in accord with the fact that the count;L: rate of the 1.hie1ded
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( re' ri
o ve7/114 r?4 t
C pY To0N s pvc6
SOU 7/4" /I 71..44 itc
- 10 -
0-M counter was rather low at the per tin time. intervals
(FiC.3)
ity with enereeies in excess of '50 key over the South ?Atlantic
maEnetic anomaly as measured by using .- the "CO;17140J ?31 aatel-
lite for the ..period from April 24 to May. 10,1962. The height
of the cross-section surface ?is approximately 650 km. The
?las 4 and 5 show the isolines of electron flux intens-
valus Indicated close to each isoline are
units of the omnidire/tional electron flux
multiplied by 6.104.
The isolines ehown in Fig 4 were obtained by using
the records taken during the periods when the magnetic
IC-index Wzs below 4 while the lines reprosente3 in Fig. 5
'take into account also the results of measurement taken at
A 4
Then taking into account the satellite revolutions
measured during the periods with large li:e-index values, the
intensity isolines become more curved and displaced. The
obeerved displacement or the isolines does not necesaarily
indicate the increase or decrease of the total amount of
electrons trapped by the geomagnetic field. It may also be
due to the height fluctuations of the surface these particles
are drifting over or due to changes in their composition and
energy spectrum.
expressed in the
-1
(cm-2 sec) when
*/ The E.7.indeX valUes are taken from the data obtained by the
Moscow station (I=IRAN).The satellite revolutions at '4
refer to May 5-6,1902..
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-.5imi1ar cross-sections p/otted by uaing the data
obtained from the sLielded GM counter. which records mainly the
protons possessing, the energies in _exCess.of 50 eysarfllue
rated in a separate report /a/. The -shape of isolines and .
the maximum flux intensity re.gions of thee.,t1p...,2x.oup.s_of
rf,,,,???????1.. foga,.
particles are di fferent.
? ???,??????? VICW W..?? 1
thi ri7e4 7tVet4 it is. rather difficult to distinguish between the space.
,,Itirpwr?-.
and time variationa (and.. the results' obtained are'not always
single-yalued). 'For better presentation of the values actually
obtained during different sataIlite revo/utions, 0 Figs,6 and
.7 show maximum flux intensity points obtained by?using the
fluorescent-screen Indicator data (blank circles) and the G-M
counter data (solid circles) with the altitudes indicated in
the graphs in km. Dashed lines refer to the satellite revolut-
'ionswith K 4 . (3ee. Pig.5). Apparently, the relative
disposition of corpuscles of different.groups.varies.even fnbm -
one satellite revolution to another, it is possibly due to..
certain peculiar 'characteristics or the Couth 4t1antic geomag,
netic anomaly region.
Table I gives Some data on the corPuscular radiation
intensity at rather low altitudes within the49' latitude..
44
The tabulated data 'indicate that predominant at low' altitudes
are not the protons with energies mev,but some other
corpuscular radiation of. lower energy.
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-12 -
3amp1e 21uxes Registc:red at Particular Locations.
-2 -1
P - omnidirectional number flux in particles cm sec ;
-
- omnidirectional energy flux in erg cm-2 sec'
Time
Coordinates
km. degrees degrees
Type
of particles
Protons
50 Lev
(omnidi-
rectio-
nal )
aectrons
oo 100kw
(omnidi-
rect io -
nal)
e ctrons
5 key
(assuming
isotropic
distribut-
ion and
= key)
3 Eai 1952
num-
19 h 02 m her
flux -
.C;n7 1470 ' .47 S 37 W .
150 ,107
1.10
,ener-
EY
flux
1,2.1072
5
0.8
num-
ber
flux
1520 19 S ? 10 13
;820
7.10rt
2.108 ?
ener-
gy
flux
P 6
-
.5.102
10
1.6,
,
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,
- 13 -
Captions to Figures
Pig. l. 2;xaaole of Recording of Soft Positive Ions by Using
Artificial Earth Satellite "COSMOS 3" on Apeil 25,1952.
Satellite orbita are shown by dashed lines and regions
of recording positive ions - by solid lines. Figures_
at ends of solid lines indicate altitudes in km.
2igures in circle-numbers of satellite revolution ?
Shown at the right side are the same regions of
positive ion recording, with the longitude transformed
into the local time.
Fig.2. Record Pattern Obtained by "COSMOS 5" Satellite by
Usin Electron Indicator with Foil 0.4 mg cm-2 thick.
Signal modulation by stepped accelerating voltage
is evident.
Fig.3. Pattern of Signals from GV Counter (solid line)
and Electron Indicator (dashed line)
Y-axis shows GM counter counting rate in logarithmic
scale. Electron indicator readings are given in arbitra-
ry units. Zaximum flux of electrons is 1.5.105 'elec-
. -1 -
trons cm sec. sec steradian1 in case their energy
E.= 50 key.
F1g.4. Intensity Isolines of Electron ?luxes over South
At/antics for Moments witil Low Geomaznotic.Activity
( X < 4 ? Unit$ are as shown in Pig.5.
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Fl
5.
? 14 ?
Intensity Isolin-to of Electron fluxes over South -
Atlantics. Intensity values near isolines are
? ?1
ex:pressed in units of 4?10 24 particles cm sec.
steradian-1 assuming electron energy equals 50 key.
5 and. 7. Zutual Arrangement of aadiation Intensity
faxima Recorded with CI Counter (solid circus) and
Electron Indicator (blank cirolesl. 1:ach point is
accompanied' by height value in km of appropriate
maxiium. .
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- 15 -
References
1. Upp4,11. Atmosphere Research by Usinz Artificial 7iarth
L'etellites 3:L0S 3 and C=OS 5. I.Yu.I.Galperin.
V.I.Erassoysky. ,i4quipmQnt.
2. V.I.Arassoysicy,Yu.Y.Eushnir, G.A.Bordoysky, G.F.Zakharev,
n.111.Svct1itaky. Detection or' Corpuscles ny Using Third
Earth Satelite. N 2, 59-60,1955.
V.I.Erassovski,YuX. Zushnir,O.A.Bordovsky, G.F.Zacharoy,
jA.3vet11t3ky. Artificial 3arth Satellites, 2, Plenum
York,pp.75-7791960?
3. V.1...Eressovaky, I.C.Shkloysky,Yu,I.alperia.3vetlitsky.
Detection of Uectrone with Znerzy Approximwte/y 10 key
in Upper Atmo,Iphere by Usini:; Third Zarth Satellite.
Doklad of the Academy of 3ciences of the U3SR,127, No.1,
78,1959.
4. V.I.4raasovsky,I.S.4J1k1oyaky, Ya.I.Galperin, i.. 3vet-
1itsky, Yu.N. Zushnir, G.A.?Bordoysky. Detction of laectrons
: with Bnergy Approzimately 10 kev in Upper Atmosphere..
Iak. &put .2;etr;li, N 8, 113-125,1961.
V.I. Arassovaky, 1. S. fihkiovsky, Yu Galperio Yu. I shnir,'
G.A.3ordovsky,1951,Artificial arth Satellites,Plonum
Press Lac.-New York,137-155,1951; P1an.Sp.Sci.,0 , 27-40,
1962.
5. B.J.0c3rien.Direct Cbservations of Dumping of Zlectrons.
at 1300-ki1ometer Altitude and 'Ugh Latitudes. Journ.
..geophys.aes., 67, No. 9,1227-1233,1962.
?
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Declassified in Part - Sanitized Copy Approved for Release 2012/12/13: CIA-RDP80T00246A022400050001-7
16 ?
6. 2.J.O'3rien?T.4fetirra of Outer?Zone z`Zectrons and Their
.'Teol?pitation into ti Ltrnospbere. Journ.Geophys.Res.,
67, lio.10, 3587-37C5,1962.
7. ::i.J.0-3rien.aeview of Ltudiect of %Trapped hadiation -with
atellite?Borne Apparatus. Space 3ci.4iev., 1, rio.3,
415-484,1963.
3. Uppr Atmo4.iphtire ResLearch by Usinz 4rtificial .1:arth
atellites "COL'MG3 3" and "COMOS 5" 2. V.ViTerriny?
High?.3nergy CorpuEz;cles.
(
?
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+3
+20
+10
0
-10
-20
-3000
\
?
r,
\
?
?
?
N.
0 % %
%337
\
? %
??
?
`. ? .
389
?
?
??
?
? 0
1
?,
387
?
?
?
?
?
?
.
?
\
?
?
?
\ 0
S.
\,402 ? \412
o
?
\471
? ?
\ ? ?
460
\
?
?
? ? ? ?
, ?
\435..
\466
? ? ? . ?
?

..,
?
?.
? ?
+600
+120?
Paper II, ic. 1.
+30?
+20
+10
0
-10
-20
30
+180? A 11
30m 12h
30m
13h
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11 kV
11 kV
?
? 6 kV
0.15 kV : ? 3 kV 0.15 kV.
ta.
4
t (see) 40 32 24 16 8 0
Paper II. Fig.2
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4-1
Ca H
1000'-
W C
O co
O 4-, 100
O g
O 0
O o
????? 10
1
10 20 30 40 50 60 70 80 t (minutes)
dayside ---1,4*--nightside-0401dayside.
220 300 500 600 700 600 500 300 h (km)
11?N
45?S
42?S
20?S
127?E
165?W
105?W
75?W
Paper II. Pig.3
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o?
00
+20?
o?
-20
-40?
6-Z?. 7,l'o ?;, > o- fr.4 V
_600
-60
o?
-20?
-40?
Paper EI; Fig. 4
o?
0
30?
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9.1 00
0
CY')
1
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+120?
180?
-120?
-60?
Paper II, Pig. 6.
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+1200 180? -120?
F
I
-60?
Vt --- _714
1J
600 680 691 16i99
?94?4146-44142:-7i----3
690
69' ? ?
-300
1
699 683
693
el2 692 -20
2
GTO 66?
?69 669
655 e/
+120? 180
Al
-120? -60?
Paper II, Pig. 7.
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STAT7
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?
TT
_
3 and .CO;3 5.
3..ForpuiJoular .aadiation
0,
,..itutoa of Atmospherie
Academy of Sciences., L:':JLicol',1*
3t1
s.;
and"Cos:no s arti.7 Le Ia.,. L
.carr.Led gasg(.-.-iE,rer of CT,7-5
- 2
3.4 ,Pb + 0.8 t;;:./..;-1a2 LI c-..,:oording of er,trat-
in rai%, 1 ' dint: reduce ,Ae nlber of .
rada. ertin C;;:nificant count
T?
tc ange of elrons in tIi! co:.-4)oite ?
convenient tc replace it by an aluminium sLF!,,
2
,..tck,which possesses an equivalent absorbin,
,power,ii va-lue corresponds to the extrapolated .range of
electonL &nd the 50 % trnzmissipon thickness for
Me . bremsstrahlunL contribution from. electrons
? Lth than 10.8 :ley is determined using the
(Piga). The left-hand scale of the
ad:5 calculated efficiency of the' geiger counter, .
8 . (i.e.. the ratio of V- coting rat sus
to numb,,tr of electrons incident to 1 j w hi' .
.X?aXiS shows the energy in key. .r, pints
obtained durin8; laboratory calibration of a Si mi I a r counter
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2
are also shown. The curve bend within the energy region
of 1.5 to 2 Mev demonstrates the rrowth of the brems?
strahlung intensity for such penetratinc through the
satellite aluminium shell and are slowed down in the lead
sield and other structural elements of the satellite with
intermediate Z. The counter efficiency curve may be used
for determining the flux of particles N () per cm2 per
sec. of energy ::: which results in a particular counting
rate. ?or example, a flux at which the counting rate equals
500 counts/aec is determined using the right?hand scale of
Y?axis (ig.1). 2xvtons penetrate through the same shield
beginning from energies of (N' 50 Mev.
The results of counting rate measurements permit
dictinuishing two regions around the 3arth : I ? a shell
close to the Earth where the counting rate varies from 1.5
counts/sec at the gecmai-netic equator to 15-20 counts/sec
at .geomagnetic invariant latitudes of 600 */.; II ? region
of penetrating radiation with a sharp lower boundary where
the counting rate exceeds 25 counts/sec. This region hos
been identified within latitudes of * 500. No systematic
growth of the counting rate has been recorded within re-ion I
Hereafter"geomagnetic invariant latitude" is defined as an
angle between th,,, radius?vector of the point in space from the
counter of the dipole and the equatorial surface (at the same
value /I-3/) of the real geomagnetic field computed in [6].
The angle lies in the geomagnetic meridian plane.
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? 3 ?
(at low counting rates) during the ascent along the line
of force,which means that the majority of the particles
recorded are ncbt trapped. Let us consider the cosmic ray
contribution to the measured counting rate. The primary cosmic
ray intensity varies from 8.3 x 10 -1 particles cm-2 sec-1
stored at geomagnetic equator to 1.5x10 particles
-1
cm sec sterad at 51? latitude [I] . iUth a mean counter
geometric factor of 25 cm2 sterad for isotropic radiation
assuming no shower formation the counting rate should vary
from 0.2 counts/sec to 3.8 counts/sec between the equator
and the 51o latitude,which is 5 to 10 times as low as
recorded counting rate. Luch an excess of the recorded count-
ing rates over the "cosmic ray background" may be due to
showers frem primary cosmic ray particles formed in the
satellite body. A similar counter with 5 g/Cm2 shielding
installed in the third Soviet space vehicle /2/ recorded
minimum counting rate of 3.2 counts/sec in the equatorial
region at similar altitudes, i.e.twice as high as that
recorded by the satellites. "Cosmos 3" and "Cosmos 5". This
may be accounted for by differeht conditions of shower
formation in the satellite body.
, Now coasider. region 11 where the counting rate grows
from 25 counts/sec to 500 counts/Sac and up. The recorded
radiation is trapped by the geomagnetic field since :
I) in most cases It ,was observed that the counting rate
undergoes modulation by /a factor of several times with the
r ,? ? ; ,
"
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4
satellite rotational half?period due to different shielding
(from maximuM of about 25 gr/cm2 to minimum of 4.2 gr/cm2)
s well as due to change of the counter axis orientation
with respect to the line of force;
2) radiation intensity varies systematically, along
the line of force.
Les us consider the co7iposition of the radiation
recorded by the counter in this region. ?ig.1 shows that
the counting rate of 500 coants/sec may be due to 1 Yev
electron flux of 1.2./0 particles cm-2sec-1
or by even
higher electron fluxes of lower energies. aince fluorescent ?
?screen indicators at that time recorded no such high electron
fluxes, it may be concluded that the contribution to the
count in rate of 500 counts/sec of the bremsstrahlung from
the electrons of less than 1 Mev is significant. Cimilarly,
for croating the same counting rate the monochromatic flux
of 3?ii:ev and :al 5?:ilev electrons (which still cannot penetrate.
throuLJI the shield into the counter) should be of 4 x 106
? ?2
part. cm2 sec-1
and 105 part. ?cm sec-1 respectively.
Llectrons possessing ouch energies penetrate through the
walls of the fluorescent?screen indicators and can be detected.
in many cases the fluorescent?screen indicators displayed no
signals at the times of the geiger countinz; rate of 50
counts/Sec. Cine their detection threshold for electrons
of such energies is below 104 part. cm-2 sec., the above,
mentioned fluxes would have certainly been detected. It
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5
VFW
. becomes evident, therefore,that the counting rate is the
region where trapped particles are present,is caused mainly
by' penetrating corpuscles. Since none of the measurements.
taken as far away as several thousand kilometres from the
Earths surface in latitudes up to 40? recorded electrons
possessing such a penetrating power, the conclusion may be
drawn that tha counter records mainly penetrating protons.
From the results obtained by.Preden and White /3/ and by
Jraugle and Zniffen /4/ it may be deduced that within the
comparable region of apace the trapped proton flux with .
energy exceeding' 50 nev reaches 40 part. cm-2sec-1 sterad.
With the counter geometric factor of .25 cm2 sterad the
counting rate should be. approximately 1000 counts/sec. which
is close to. the value recorded. .
The lines shown in Pig.2 connect points of equal
_counting rates obtained at an altitude of about 650 km over
the South Atlaatic. The shape of the isointensity curves
is quite similar to the lines for equal' values of the module
of total magnetic field_ at this altitude. /5/
To determine the .position of the trapping region
boundaries, the points of the counting rate's of 25 counts/Sec
and 500 counts/sec are plotted. in coordinates, B , where
B - the geomagnetic field vector in gauss and cib. the
latitude of the point defined Heather (Fig.3a). Values
of B. and 140 have been obtained using the data on the
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earth's field garmonic expansion with 512 coefficients /V.
The scattering of experimental points depends to a'considerable
extent on the error in determining the maximum counting rate
at deep modulation due to the satellite rotation. The mean '
curves have been drawn to describe the obtainad:distribution.
olid .line corresponds to the counting rate of 500 counts/sec,
the dashed line - to 25 counts/sec. Then these an curves
are replotted in coordinates H (rig. 3b), where H
mdnimum height above the Earth a. surface which is reached by.
the mirror Paint of.a particle drifting artiund the 2arths
These minimum heights in the Southern Bemisphere are located -
approximately along the 60th meridian, western longitude.
?igs 3a and 3b chow that the lower boundary of the
?'trapping region at latitudes up to /5? - 20? 'below. 500 km
- is determined by the atmospheric scattering .and at higher
latitudes .it runs' along lines of equal valuesof the tagnetit
field vector.
It is well known,that when d Scribing' the movement of
Charged particles in a stationary non-uniform magnetic field .
using three invariants of motion, such an :
magnetic Moment, I longitudinal invariant and ?
7- flux invariant, at least the following requirement.
should be met
Lam
R 4rad B
B
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where R
Larm
?7-
- particle Lamar radius. This reqUirement
is not met for recorded protonsta,s this value is of the
order or 0.2 for a proton energy of 130 ;,:ev. Thereforepthe
--
movement trajectc:.7 "accurately enough
using the three invariants
Pis 3a and 3b
suggest the idea that the particls might drift in the
meridional direction along /Ines of the equal value of 181.
) ,
In conc/usion the author wishes to express,his
appreciation to V.I.Erassovsky for guidance and to Yu.i..Gal?
perin for advice and direct assistance.
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fa
?
8
Figures
Fig.?. Efficiency Curve of GM Counter
Points.are Results of laboratory calibration
Pig.2. Lines of Equal Counting Rate at altitude of about
650 km in South Atlantic.
Pig.3. Locations of Equal Counting Rate 25 counts/Sec.
and 500 counts/sec.in Coordinates:
a) Bp 015 .(13-- magnetic field vector at the point
.
of measurement ; ? lb geoma8netic invariant
latitude (see text) ;
b) H. Op (14. ? minimum altitude above the :Earth's
?surface in km which ,id reaChed by the mirror point
while drifting around the Earth.
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?
Bibliography
1. A.N.Charakhchian, T.H.Charakhchian. Leasurements of
Cosmic Ray Intensity in Stratosphere. Journ.of Sxper.and
Theor.?hys.,Vo/. 35, No 5,1956,1088-1101.
2. I.A.Savenko, V.E.Nesterov, P.I.Shavrin, N.F.Piaarenko.
Cosmic Lay Equator from Data Obtained from Third Soviet
earth Satellite Vehicle. Artificial Sarth Satellites,
issue II, /961, 30-34.
3. S.C.Preden, H.S. White.,
E Journ.Ceophys.,Reg., 65, 1377-1333,1960.
4. J.2.Naug1e, D.A. Xniffen. Flux and Energy Spectra of the
Protons in the inner Van Allen Belt. Pi.lys.Rev.Let.,
. 7 , No.1, 3-6,1951. ?
5. Handbook of Geophysics., New York, p. 10-12,1960.
6. D.C.Jensen,R.W. 2urray, J.A.Welch.Tables of adiabatic
Invariants for Geoma8netic ,Field 1955. AFSWC-TN-60-81
April 1960, APS:VC-TN-60-19 August 1960.
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1
45' -
4(55-
40-4-
455 -
40-6 -
40-
A counts
pW1
rd pdt.
CM2 CC.
40
Paper 3. Fig. I .
40
-403
-10
'-404
r40?
-409
-4015
EKSV
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Declassified in Part - Sanitized Copy Approved for Release 2012/12/13: CIA-RDP80T00246A022400050001-7 ?
?
Paper III. Fig.2
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? IBI
(gauss )
0.30
0.25
0.20
(km)
1000
?1
? -- ? 25 counts sec
500 counts see-1
?
? 0? ?
et ? .......? ...we ? 46.? 0 mem
. .t...? .
oe. ?? ?
? 00. ? .$
? 11?? ?
S
e a ?
? ?? ? J????.
.. ?
? .,.? -or ? 0+ + 4, 4+
?
. .?.....s.?...-
? * _._ + ? *
.. ? ? + + v'"
? t?
* +v.+
*
t + ? ?
? 4. 4.
*
*
?
?????? =ID
? 1 ?
10 20 30 40 50
500 :'? ? .......... ? ??????
? ? ? ............. ? ?
??? OM, ...=?? ??????? OBEs ammo
.?
?,0* ? .*** 4vB=0.26
? .? n?
.?? 4??
.?? /.??
.? 13=0.20
?.?? B=0.22
.?? .? B=0.24
? ? ?
? ? ? .? ? ? ?
? ...... ? ? ? ? ? ?
???
? ? ??? ???? ?
:?.????
? ? ? ? ?
10 20 30 40 50
South geomagnetic invariant latitude lr
Paper III. Pig.3
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STAT
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?
S N. Verney , I . A. Savenko P . I . Shavrin
L.V.Tversk,aya
THE EARTH ADD RADIATION BELTS STRUCTURE AT AN ALTITUDE
OP 320 1410LTTRIM
Abstract
According to the 2nd Soviet Spaceship-satellite data,
the intensity distribution in the radiation, belts on the
drifts shells at an altitude of 320 km was studied.
The dependence of intensity on longitude, for various
values of shell liparamfter has been obtained.
The chance of intensity as a function of longitude has
been discovered along the lines of equal E (B denotes magnetic
field intensity).
The connection of intensity with the structure of the
real geoa etic field has been traced, The temporal intnns-
ity variationd are also discussed.
?????????????61,.,?"
Analysis of spatial, intensity distribution in the radio-
active belts at low altitudes is considerably hard to carry
out because of quite a nubber of circumstances. The fact,
that the geomagnetic field is not that of a dipole causes an
adverse effect at low altitudes. Whereas for the central di-
pole the equal B line at all longitudes is located at an
uniform altitude, this altitude strongly depends on longitude
for the real!geomagnetic fields By this reason while their
longitude drift the particles come to regions of significantly
variable atmlospberic, density. As aa example we can point out
that the altitude of mirror points in the South hemisphere
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? G.
- 2-.
varies by more than 1,000 km depending on longitude, while
the atmospheric density, according to / I /10 varies by e
times at a distance of 100 km, Since atmospheric density
at low altitudes is high the mean particle, lifetime, related
to the downward diffusion can be shorter then a longitude
drift period. This will lead to the appearance of longitude
dependence (longitude dependence is understood as a dependence
of the intensity along the equal B lines on longitude).
In the presence of the longitude dependence the methods
of presenting results in MoIlwaints two-dimensional coordinate
system 11, L / 2 / is naturally inapplicdble as in this case
different intensities from different longitudes will. corres-
pond on the graph to the point with given B, L.
The results obtained at the 2?,nd Soviet spaceship-satel-
lite / 3 / show planetary intensity distribution registered
by luminescent counters at an altitude of 320 km and enable
to trace longitude intensity dependence on different drift
shells.
To a drift approximation the leading centre of a charged
particle moves in a magnetic trap on a surface which consists
of the pieces of magnetic force lines and is determined by
the conditions of constancy of magnetic moment and of longi-
tudinal invariant
where the integral is taken along a magnetic line of force
between the reflection points 1 and l*, and B3 is field
intensity in mirror points*
Generally speaking, in an asymmetric field the drift sur-
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?
?
fazes eg to avtiolea initialij cated on the 4am3 r.a7,netle
fcroellno nay-fail to eolnaidee "le Ilvaln Pi, however, on
? tao og fs;lpherloal cmay$143 data aowea tht gor?th0
, actual gocrinctio?field this e':aect 10 noclicAble0 CoBsevent
there cmlot2.n13 oarfven in 441,e geemaznet13? acid whle4 arc
formed.zieefic
. S xpucmane (108 9/46'X) um ri/CeR)
? 4-.4. -......r.
-.1???? 0). Oo CZ) N.,
- 20. X1
- 24. X1
1\)
(71
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-25.1
CA)
1--X
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H
10 20 30 10 20 30 10 20 30
moR5pb 1962 r geKab-pb 1962 r. fitiBapb 1962?r.
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(tit
C.)
< (tf
19.5- 3000
196'
19.0 -
18.5
2900
-4
/c)?
0
cpeaHee no
// P TisgiffiblM ny111,1-4
t.,rnparnocpepa
5 6 7
8 9 10 11 /2 13 14 /5 16
Anpen b 1963roga
Acme
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-4,7 4v
? 12-10
3
15 20 25 20 35 40 NT Am
20.40
21.20
21.40 22.00 t F. /9
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?
/
10I
Mtpc-J 2 mocmutiectfan pager?
SZVaarommaporamarshavw.?.???????s???????????????????
10 11 /2
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