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
Radiation Storms in the Near Space Environment
Mikhail Panasyuk,
Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow
State University
Solar storms,
Radiation storms,
Geomagnetic storms
Intensification of solar activity
Radiation storms in several 100’s keV particles flux variations
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
Galactic cosmic rays
Solar energetic particles
Radiation belts
Earth’s radiation environment
• SONG (Solar Neutrons and Gamma- rays)
• MKL (Monitor of the cosmic rays)
• SKI-3 (Cosmic ray nuclei detector)
Energetic particles instruments onboard Coronas-F
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
CORONAS – F gave us new results on:
- SEP generation during solar flares;
- SEP penetration;- dynamics of proton and electron radiation belts.
Galactic cosmic rays
Earth’s Radiation Environment
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:
Solar energetic particles
Earth’s Radiation Environment
SEP radiation storm• Acceleration at solar flare site;
• Propagation in IPM with modulation, acceleration by CME shocks;
• Penetration inside the magnetosphere and
partial trapping(?)
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
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
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
October- November’03 radiation storm CORONAS-F / solar gamma-rays,neutrons
The first phase Shock-wave acceleration
The second – delayed phase Pion-decay production
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
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
SEP penetration
October- November’03 Radiation StormSEP penetration at low altitudes
– low-latitude boundary of
SEP penetration
b
Satellite’s orbit
SEP
Transmission function during quiet/stormymagnetosphere
Effective rigidity of penetrating particles decreases during magnetic storm periods
b
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
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
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
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
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
Radiation belts
Earth’s radiation environment
October- November Radiation Storm
Electron radiation belts
Radiation belt dynamics
Dynamics of relativistic electron belts
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
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
SEP trapping
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
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
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
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
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
Geostationary radiation storms
vs LEO polar
radiation storms
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
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
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
SEP doses effects
October- November Radiation StormISS dosimetry
ISS/SRC,R16 data,
SINP, IMBP
October- November Radiation StormISS dosimetry
ISS/SRC,R16 data,
SINP, IMBPR16
DB-8
October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data
October,03
Solar particles dose effect : 140mrad
ISS
October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data
October,89
October,03
Solar particles dose effect : 140mrad
ISS
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
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
Conclusions
• SEE for LEO:-Intensification of electron component of RB &-Enhancement of proton (ion) fluxes due to
SEP penetration
Thank you
The new proton belt formation
Polar LEO flux
GEO fluxDst
Polar LEO radiation storm at low latitudes
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
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
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 :
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 ?