radiation storms in the near space environment mikhail panasyuk, skobeltsyn institute of nuclear...
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Radiation storms in several 100’s keV particles flux variationsTRANSCRIPT
![Page 1: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/1.jpg)
Radiation Storms in the Near Space Environment
Mikhail Panasyuk,
Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow
State University
![Page 2: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/2.jpg)
Solar storms,
Radiation storms,
Geomagnetic storms
Intensification of solar activity
![Page 3: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/3.jpg)
Radiation storms in several 100’s keV particles flux variations
![Page 4: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/4.jpg)
Topics to search Where are these guys from? - radiation belt; - SEP events; - ionosphere
What kind of physical mechanisms for acceleration and transport are dominated during extreme events?
- radial diffusion; - local rapid acceleration; - injection ; - local losses
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Galactic cosmic rays
Solar energetic particles
Radiation belts
Earth’s radiation environment
![Page 6: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/6.jpg)
• SONG (Solar Neutrons and Gamma- rays)
• MKL (Monitor of the cosmic rays)
• SKI-3 (Cosmic ray nuclei detector)
Energetic particles instruments onboard Coronas-F
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CORONAS-F:MKL,SKI, SONG, instruments:
Electrons ~ 0.3 -12 МeV &
Protons ~ 1 - > 200 МэВ
Ions р -Mg with 2 -30 MeV/nucl X, gamma –rays with ~ 0.03 - 200 МэВ Neutrons
Skobeltsyn Institute of Nuclear Physics
![Page 8: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/8.jpg)
CORONAS – F gave us new results on:
- SEP generation during solar flares;
- SEP penetration;- dynamics of proton and electron radiation belts.
![Page 9: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/9.jpg)
Galactic cosmic rays
Earth’s Radiation Environment
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299 300 301 302 303 304 305 306 307 308 309
Д н и 2 0 0 3
1E-4
J(p>
700М
эВ)
7000
8000
9000
10000
N/1
00/ч
(S. P
.)0.02
0.03
0.04
J(p>
75М
эВ)(
L=1.
5)
0.030.040.050.060.070.08
J(p>
75М
эВ)(
L=2)
1E-1
1E+0
J(p>
75М
эВ)(
L=2.
5)
1E-1
1E+0
J(p>
75М
эВ)(
L=3)
N (S .P .) p > 7 0 0 М эВ
L=1.5
L=2
L=2.5
L=3
Cosmic rays inside the magnetosphere
Oct-Nov’03 event :
-SEP: increasing;
-Forbush effect up to ~ 30%
-Semiduirnal variations up to ~10-15 %.SP NM
GOES
Coronas-F
GCR:
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Solar energetic particles
Earth’s Radiation Environment
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SEP radiation storm• Acceleration at solar flare site;
• Propagation in IPM with modulation, acceleration by CME shocks;
• Penetration inside the magnetosphere and
partial trapping(?)
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1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
Час
тицы
/ с
см^
2 с
р
1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5Ч
асти
цы /
с с
м^2
ср
26 27 28 29 30 31 01 02 03 04
p3
p2
О к тя б р ь - н о я б р ь 2 0 0 3 U T
Ю
С
Ю
С
2,3-4,2 MeV/nucl
4,4-19 MeV/nucl
H
He
H
HeShort time delay,quick-time
front, large anisotropy and absence of dispersion
(during ~12 h). Λ is large
AR 484
Oct. – Nov.’03CORONAS-F data
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1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
Час
тицы
/ с
см^
2 с
р
1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
Час
тицы
/ с
см^
2 с
р
26 27 28 29 30 31 01 02 03 04
p3
p2
О к тя б р ь - н о я б р ь 2 0 0 3 U T
Ю
С
Ю
С
2,3-4,2 MeV/nucl
4,4-19 MeV/nucl
H
He
H
HeFree particles propagation
withmodulation by a shock wave
AR 486
XRS Data
1E-07
1E-06
1E-05
1E-04
1E-03
1E-02
28 Oct 29 Oct 30 Oct 31 Oct 01 Nov
Date
G12
Xra
ys .
1-.8
A
X
M
B
C
Oct. – Nov.’03CORONAS-F data
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1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
Час
тицы
/ с
см^
2 с
р
1E-1
1E+0
1E+1
1E+2
1E+3
1E+4
1E+5
Час
тицы
/ с
см^
2 с
р
26 27 28 29 30 31 01 02 03 04
p3
p2
О к тя б р ь - н о я б р ь 2 0 0 3 U T
Ю
С
Ю
С
2,3-4,2 MeV/nucl
4,4-19 MeV/nucl
H
He
H
He
2 –days flux increase, diffusion propagation,
Λ is extermely small
AR 486
XRS Data
1E-07
1E-06
1E-05
1E-04
1E-03
1E-02
28 Oct 29 Oct 30 Oct 31 Oct 01 Nov
Date
G12
Xra
ys .
1-.8
A
X
M
B
C
Oct. – Nov.’03CORONAS-F data
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October- November’03 radiation storm CORONAS-F / solar gamma-rays,neutrons
The first phase Shock-wave acceleration
The second – delayed phase Pion-decay production
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18.0 18.5 19.0 19.5 20.0 20.5 21.0D ay o f January
1E-1
1E+0
1E+1
1E+2
1E+3P
(50-
90 M
eV),1
/s C
OR
ON
AS
-F
1E-3
1E-2
1E-1
1E +0
1E +1
1E +2
1E +3
P>5
0 M
eV G
OE
S-1
0
GOES-10 p>50 MeV
CORONAS-F p 50-90 MeV
Тatiana
radiation storm 20.01.05Tatiana
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06:44 06:48 06:52 06:560
3000
6000
9000E 0.15-0.5 MeV
E 60-100 MeV
Time, UT hh:mm
0
5
10
15
20Phase IIPhase I
Две фазы вспышки в - излучении. Tatiana radiation storm CORONAS-F / solar gamma-rays,neutrons
Gamma –rays with > 60 MeV as a result of interactions of > 200 MeV protons
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SEP penetration
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October- November’03 Radiation StormSEP penetration at low altitudes
– low-latitude boundary of
SEP penetration
b
Satellite’s orbit
SEP
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Transmission function during quiet/stormymagnetosphere
Effective rigidity of penetrating particles decreases during magnetic storm periods
b
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SEP penetration at low altitudes300 301 302 303 304 305 306 307 308
Д н и 2 0 0 3
1.5
2.0
2.5
3.0
3.5
L
-1 .70
-1 .60
-1 .50
-1 .40
-1 .30
-1 .20
-1 .10
-1 .00
-0 .90
-0 .70
-0 .50
-0 .30
-0 .10
-0 .00
0.10
299 300 301 302 303 304 305 306 307 308 309Д н и 2 0 0 3
-400
-300
-200
-100
0
Dst(н
T)
3
4
5
6
7
L
October- November’03 Radiation Storm
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October- November’03 Radiation StormSEP penetration at low altitudes
50
60
70
Инв
. шир
ота
О к т я б р ь - Н о я б р ь 2003
0
200
400
Kp
Kp- dependence
Evening
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October- November’03 Radiation StormSEP penetration at low altitudes
50
60
70
Инв
. шир
ота
О к т яб р ь - Н о я б р ь 2003
N SГ р а н и ц ы п р о н и к н о в ен и я С К Л (р : 4 .4-19 М эВ ) в п о л я р н ы е ш а п к и в в еч ер н и е ч а сы : ,
-400
-200
0
Dst
Dst -dependence
Evening
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October- November’03 Radiation StormSEP penetration at low altitudes
0 30 60 902
4
6
0 30 60 9010Kp
3
6
93
6
9
12
15
3
6
9
6
12
18
24
30
L
6121824303642L
M L T = 6 -9 ч M L T = 1 8 -2 1 че (0 .3 -0 .6 М эВ )
р (1 -5 М эВ )
р (5 0 -9 0 М эВ )
MLT - dependence
-400 -300 -200 -100 0D st(н Т )
3
6
9
-400 -300 -200 -100 02
4
6
3
6
9
3
6
9
12
15
6
12
18
24
30
36
42L
6
12
18
24
30
L
Morning Evening Morning Evening
Kp Dst
Neither Kp or Dst indexes are not representative
for a global distributionof SEP penetration
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October- November’03 Radiation StormSEP penetration at low altitudes
Coronas-Fdata, Skobeltsyn Institute of Nuclear Physics
Variation of proton penetration boundary during isolated substorm
Substorm activity as
a regulator of SEP’s
penetration
![Page 27: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/27.jpg)
Radiation belts
Earth’s radiation environment
![Page 28: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/28.jpg)
October- November Radiation Storm
Electron radiation belts
Radiation belt dynamics
Dynamics of relativistic electron belts
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October- November Radiation Storm
Coronas-F data, Skobeltsyn Institute of Nuclear Physics
Energetic electrons & protons dynamics /Coronas F data
Redistribution plus acceleration of energetic radiation inside
the traping region
Oct.,29
Oct.,28
Electron radiation belts
Inward movement of RB
![Page 30: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/30.jpg)
300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г .
L
lgJe(0
.3-0.6
МэВ
)
L
lgJe(0
.6-1.5
МэВ
)
L
lgJe(1
.5-3М
эВ)
8.5
4.0
2.4
1.7
1.3
1.18.5
4.0
2.4
1.7
1.3
8.5
4.0
2.4
1.7
1.3
1.1
1.1
Electron belt variations
300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г .
-400
-300
-200
-100
0
Dst(н
Т)
3 phases:
SEE injection,depletion,
thennew RB formation
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SEP trapping
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Ejection of SEP inside the RB really exists
Solar energetic particles as a source of RB population
10 MeV protons There are some doubts that this source is important for the quiet-time structure of
the RB
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Solar energetic particles as a source
of RB populationOne should expect the life-time of SEP particles to be very small because of their high rigidity (see Alfven criteria).
Therefore, the probability of observing SEP particles inside the RB is small
Criteria for stable trapping:
L/M ~ LB/B= <<1
L - larmour radius, M –magnetic field line curvature, B - magnetic field magnitude
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2 3 4 5 6 7 8 91 10L
1E-1
1E+0
1E+1
1E+2
1E+31E-1
1E+0
1E+1
1E+2
1E+3
1E+4J (с м 2 ср * с )-1
06.1105.11
07.11
12.11
p (1 -5 М эВ )
р (1 4 -2 6 М эВ )
С П
Proton belt variations
2 3 4 5 6 7 8 91 10L
1E-1
1E+0
1E+1
1E+2
1E+31E+0
1E+1
1E+2
1E+3J (с м 2 с р * с )-1
23.1125.11
30.11p (1 -5 М э В )
р (1 4 -2 6 М эВ )
С П
The new proton belts
6-12.11.03 23-30.11.03
Impulsive acceleration or nonadiabatic process?
> 1MeV
>14 MeV
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300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г .
L
lgJ(
e>1.
6;p>
23М
эВ)
L
lgJp
(14-
26М
эВ)
L
lgJр
(1-5
МэВ
)
4.0
2.4
1.7
1.3
1.14.0
2.4
1.7
1.3
1.18.5
4.0
2.4
1.7
1.3
1.1
Proton belt variations
300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г.
-400
-300
-200
-100
0
Dst
(нТ
)
2 phases:
-SEP injection, then-new proton belt formation
![Page 36: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/36.jpg)
300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г .
L
lgJ(
e>1.
6;p>
23М
эВ)
L
lgJp
(14-
26М
эВ)
L
lgJр
(1-5
МэВ
)
4.0
2.4
1.7
1.3
1.14.0
2.4
1.7
1.3
1.18.5
4.0
2.4
1.7
1.3
1.1
Proton belt variations
300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г.
-400
-300
-200
-100
0
Dst
(нТ
)
3 phases:-SEP injection,-depletion, then-new proton belt formation
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Geostationary radiation storms
vs LEO polar
radiation storms
![Page 38: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/38.jpg)
298 302 306 310 314 318 322 326 330D O Y 2003
1E -1
1E +0
1E +1
1E +2
1E +3
1E +4
1E +5
1E +6
1E +7P
roto
n flu
x 1/
(cm
**2
s sr
)
C O R O NAS-F
p1-5 M eVp 14-26 M eV
p 50-90 M eVp 26-50 M eV
-500
-400
-300
-200
-100
0
Dst
Coronas-F
Daily averaged data
![Page 39: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/39.jpg)
298 302 306 310 314 318 322 326 330D O Y 2003
1E -2
1E-1
1E+0
1E +1
1E+2
1E+3
1E +4
1E+5
1E+6
1E +7П
оток
и пр
отон
ов, 1
/(cм
**2
с ср
)
-500
-400
-300
-200
-100
0
Dst
p 14-26 C O RO NAS-F
L<2.5L 2.5-10L>10
GOES Inner zone
Solar protons cause radiation storms at LEO
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Intensity of radiation storm at LEO polar orbits on daily averaged time scale is mainly dependent on SEP penetration
at low latitudes than on effects of RB’s particles redistribution or (and)
acceleration at low latitudes
![Page 41: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/41.jpg)
SEP doses effects
![Page 42: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/42.jpg)
October- November Radiation StormISS dosimetry
ISS/SRC,R16 data,
SINP, IMBP
![Page 43: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/43.jpg)
October- November Radiation StormISS dosimetry
ISS/SRC,R16 data,
SINP, IMBPR16
DB-8
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October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data
October,03
Solar particles dose effect : 140mrad
ISS
![Page 45: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/45.jpg)
October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data
October,89
October,03
Solar particles dose effect : 140mrad
ISS
![Page 46: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/46.jpg)
October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data
October,89
October,04
Solar particles dose effect (total): 3070mrad
Solar particles dose effect : 140mrad
ISS
MIR
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0
5
10
15
20
25
30
35
40
0 90 180 270 360Долгота восходящего узла орбиты, градус
Доза
за
сутк
и, м
Грей
.
SPE oct 28SPE oct 29
Calculated ISS doses vs initial orbital parameters
Oct., 28, 2003
Longitude
Dose
DB-8 detector onboard ISS
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Conclusions
• SEE for LEO:-Intensification of electron component of RB &-Enhancement of proton (ion) fluxes due to
SEP penetration
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Thank you
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The new proton belt formation
![Page 51: Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University](https://reader035.vdocuments.net/reader035/viewer/2022062523/5a4d1ad17f8b9ab0599716ae/html5/thumbnails/51.jpg)
Polar LEO flux
GEO fluxDst
Polar LEO radiation storm at low latitudes
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298 302 306 310 314 318 322 326 330D O Y 2003
1E -2
1E-1
1E+0
1E +1
1E+2
1E+3
1E +4
1E+5
1E+6
1E +7
Пот
оки
прот
онов
, 1/(c
м**
2 с
ср)
-500
-400
-300
-200
-100
0
Dst
p 1-5 C O R O N AS-F
L<2.5L 2.5-10L>10
Inner zone
Solar protons
GOES
Daily averaged
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Conclusions
1.Solar extreme events (SEE) can really cause the drastic
changes in the earth’s radiation environment, but
their value depends on their geoefficiency
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Bengin,et al,1992
Mir doses during the solar flares
Doses increased in severaltimes because of penetration
of SEP at LEO.
Kp
«Mir» data
October 19, 1989 :
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ISS doses during Oct.- Nov.’ 03
0.0
0.5
1.0
1.5
2.0
2.5
3.0
3.5
4.0
4.5
5.0
28 î êò 03 29 î êò 03 30 î êò 03 31 î êò 03 01 í î ÿ 03Time
Accu
mul
ated
dos
e, m
Gra
y .
Meassured data
CORONAS_&_L
CORONAS_&_Dst
GOES_&_L
GOES_&_Dst
LEO – GEO measurements disageement ?