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AUTHORSi
'
Mishin, V. M., Naydenova, N. Ya.,
Platonov, M. L.
/
TTPLEj
The diurnal variation of the probability of the appearance of the
coramencements,
the active periods and the ends of magnetic storms
PERIODICAL!
Qeomagnetizm
i aeronomiya,
v.
2,
no.
6,
1962,
110?
- 1112
TEXT;
The authors investigate the probability of the appearance of
- r
commencements,
the active periods and the ends of magnetic storms on the basis
of>,the Irkutsk Storms Catalog for 1905
-
1917 and 1925
-
1959.
The catalog
describes 8a) storms,
A tiotal of 539 of them are storms with a gradual commence^
ment.
Figure
1 presents the curves
Sh(5
(nb), San (ap) and Sa for Irkutsk,
Or-
dinates in curve
1 represent the frequencies of the commencement of the 0-storms
in curve 2
- the frequencies of the active hours n^p,
and in curve 3
“ the
equivalent amplitudes Rh.
Similar distinctions between Sa and
Sj^^j were also
observed at all bther stations.
These data,
characterizing the phases of the
maximum of the first hu^^monio of Sa and
Snt>,
are pcesented in a table.
The
authors explain these results by proposing that
Sjj'j, may be' considered as^ a re-
;
if
“
:
;
.
:>
^
-
:2
Card 1/3
^
:
'.v
.
The diurnal variation of the...'^
S/203/62/OO2/OO6/010/020
^’A 160/A 101
i. ^It of Sa.
It
is followed that the probability of
a' contact of the corpuscular
flux with the Earth does not depend on the time of the day.
This conclusion is
,
' confirmed by the fact that,
according to the mentioned catalog, the diurnal
variation of the frequency of SC practically does notpexist.
The authors then
investigate the total of all
stprfn days and introduce the following four hypo-'
theses,
1) The probability that there is a contact between the flux and the
Earth,
causing the storm is equal for all hours of a day.
2) The magnetic ac-
tivity during the hour of the commencement of the storm A is not lower than that
duri^ an average, storm X
t
A >'A.
3) The values, of A during the initial hours
i
^
of the storms are deteimilned by Sa on
Idae basis of the perturbed days,
4) The
length of each storai is
55- 12 hc^rs.
The distribution of the probabilities of
•;
the commencement of the storms over the hours of the day P
(T) will be as fol-
j
lows!
P = 0 in two 6-hour intervals T
- 900 and T > o6jj + 900 (pi^re 2i
. hatching),. P
1/24 in the
ll-houb iHiterval
+ 90°
T
>oL^ - 75°, P =13/^4
;
in one hour containing the moment
Tj^
- 90°.
Such a distribution of 'the
I
probability P
(T) has the form of a try-square shown bn. Figure
2,
The authpi^S
,
make the following conclusions,
l) It was determined! that the commencements
5 of
the storms
(recorded at the given
. station)' are generally shifted to the side
i of
j.
Cai?d., a^3
^
The diurnal variation of the . .
.
Aw^^og^o5^J(v^ao?:
dew
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n.asrteWz„a
.
an4
1 tablei
V
so AN^SSSR (institute of Ter^estrial7 ^
Kidlovoln
Pi-opagation of SO,
AS USSR)
®snetism.
Ionosphere and Radio:
SU^ITTEDj
June
23,
1962
;
SU!^ITTE33j
;
Plgdre
,j
Figure- 2.
Card 3/3
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CODE
COUNTRY
491
USSR
LOCATIOIJ
. „
JLr iCuT 5
k:
DATE/ INFO
DATE/SOURCE
DA
MO
YR
DA
MO
YR
DEC 6l
-0078>Pfb005
PROCESSING DATE
PS
AF CHART
ACTIVITY CODES
1131
I
S/T
I
NAME
OF
INSTALUTION
[
rvjfl S
CONTROL
NO.
SOURCE
CIA/OSI-RA/61-11
SCIEOTIFIC IN-EELLIGENCE EESEAECH AID
PRINCIPAL RADIOTELESCOPES OF THE 'SOVIET UNION
IRKUTSK SOLAR STATION
Alteraata Haul©:
Laboratory for Solar Study
Sufeordimte to;
Institute of Terrestrial Magoetism, Imosptere,
and Radiowave Propagation, Moscow.
In
subordinate to the Irkutsk Ionosphere-Magnetic
Station of the Ministry of Coimmnicatlons
Locatlcm;
Meget, near Ir^tsk, RSFSR
52® 28’ N-
lOlj.® 02’ E
Fimatlonal Description
Technical Description
Personalities
Other Inforamtion
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31 „ay
1951
PHENOMENA IN THE UPPER ATMOSPHERE
REVIEW OP SOVIET LITERATURE
AID Work Assignment No.
Report
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PERIOD ij
May I96I
Thit
18 the thirteenth In a monthly
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in estrophyeioe and geophyeioe.
Beginning
with thie report the eeriee identifioation
ie changed to read AID Work Asaignment No.
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The report
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on materials reoeived at the Air Information
Division in May.
Materials in this report deal with the
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II.
Solar radiation and the ionosphere
III. Van Allen belts and cosmic rays
IV. Telluric currents
V.
Atmospheric electricity
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