20 JANUARY 2005 FLARE
CORONAS OBSERVATIONS
Kuznetzov Sergey (PI), sergenik@srd.sinp.msu.ru,
Kurt Victoria, vgk@srd.sinp.msu.ru,
Yushkov Boris, clef@srd,sinp.msu.ru,
Svertilov Sergey
Skobeltzyn Institute of Nuclear Physics, Moscow State
University
Kudela Karel (co-PI) Institute of Experimental Physics, Slovak
Academy of Sciences, Kosice, kkudela@upjs.sk
6th RHESSI workshop
20 January 2005 flare
5
10
Proton onset
4
10
Counts s
-1
3
10
2
10
1
10
0
10
06:35
06:40
06:45
06:50
UT, hh:mm
06:55
07:00
Evolution of different parameters of the flare emission
The phases correspond to that of 11 JUNE 1991 flare.
Time profiles of the low and high energy gamma-ray
emission
High energy emission
is delayed compared to
the low one.
Time profiles in all the energy windows
Zoomed time profiles
0,02
6000
0.043-0.082 MeV
4000
10.8-23.2 MeV
0,01
2000
0,00
0
1200
0.082-0.23 MeV
800
23.2 -40.3 MeV
0,01
400
F, cm
-2
s
-1
MeV
-1
0,00
0
60
0.23-0.78 MeV
40
0,010
40.3-63 MeV
0,005
20
0,000
0
4
XG10
15 point AA Smoothing of RFLUX565_XG10
0,006
0.78 -2 MeV
63-93 MeV
0,003
2
0,000
0
0,4
93-155 MeV
2-6.2 MeV
0,001
0,2
0,000
0,0
0,08
0,04
0,0001
6.2-10.8 MeV
XG12
15 point AA Smoothing of RFLUX565_XG12
155-310 MeV
0,0000
0,00
06:43
06:44
06:45
06:46
06:47
UT, hh:mm
06:48
06:49
06:43
06:44
06:45
06:46
UT, hh:mm
06:47
06:48
06:49
Energy spectra in the phases
IA and IB
20 January, 2005
SPRN
IA SONG
IB
3
10
F, sm
-2
s
-1
MeV
-1
The absolute flux is compared
with that of SPRN- X-ray detector
onboard CORONAS
1
10
-1
10
-3
10
-5
10
0,01
Distinct 0 component is seen in
the phase IB.
0,1
1
E, MeV
10
100
4
4
10
10
IA
-1
10
Int-II?
IB
2
10
0
0
10
-2
F, cm s MeV
-1
2
10
-2
-2
10
10
-4
-4
1x10
1x10
-2
10
0
10
2
10
-2
10
0
2
10
10
E, MeV
-2
10
0
10
2
10
Comparison of RHESSI and SPRN time profiles
in similar energy windows.
SPRN
RHESSI 50-100 keV
48-120 keV
1000
0
8000
4000
0
-2
-1
F, cm s MeV
-1
2000
60000
SXR component substructed 8000
18<Ex<48 keV
40000
4000
20000
0
06:40
06:45
06:50
UT, hh:mm
06:55
07:00
s
0,06
-2
8
0,04
0,02
6
0
0
06:40
06:43
06:46
06:48
F cm
500
1000
0,08
HESSI 7 MeV
SONG 6.2-10.8 MeV
-1
Counts s
-1
-1
-2
Counts s
-1
2000
MeV
10
1000
F, sm s MeV
HESSI 100 keV
SONG 82 keV
-1
0,10
-1
3000
0,00
06:51
06:40
06:43
UT
06:46
06:48
06:51
UT, hh:mm
180
60
2
-1
-2
-1
Counts s
-2
-1
120
-1
40
-1
F, sm s MeV
140
Counts s
HESSI 300 keV
SONG 230 keV
-1
HESSI 800 keV
SONG 775 KeV
300
200
20
100
100
80
0
06:40
06:43
06:46
UT, hh:mm
06:48
06:51
F, cm s MeV
4
160
0
06:40
06:43
06:46
X Axis Title
06:48
06:51
January 20,2005
80
LINE 2.2 MeV
60
SONG
Arbitrary Units
40
20
0
1,6
RHESSI
1,2
0,8
0,4
0,0
06:43
06:46
06:48
06:51
UT, hh:mm
06:54
06:57
line 511 keV
RHESSI
0,5
0,0
Counts s
-1
15
E >60 MeV
E 0.78-2 MeV
60
10
40
5
20
0
0
-5
06:40
06:42
06:44
06:46
06:48
UT, hh:mm
06:50
06:52
06:54
-1
80
20
Counts s
Arbitrary units
1,0
What we see at the end of the phase IB
5 points sm 41-300 MeV
5 points sm 6.2-10.8 MeV
Count s
-1
Count s
-1
100
10
06:44
06:45
06:46
06:47
06:48
06:49
06:50
06:51
UT, hh:mm
Decay of bremmstrahlung emission becomes more steep than that of
emission. It seems that variation of the intensities becomes
asynchronious.
0
6000
5000
F,sfu
Nobeyama
2GHz
4000
3000
2000
06:44
06:45
06:46
06:47
06:48
Ut, hh:mm
06:49
06:50
06:51
Plasma temperature begins to decrease at the end of
the phase IB
The shortest path of protons L1 =1.055R
Time delay of Ep=5 GeV (Vp=0.987c)
relative to gamma-ray is 35s
Escaping time must be near 06:48 UT
Remember that 06:48 UT is the crucial point in the flare development
????

If the L>L1 than escaping time shifted to more
earlier time.

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R=0.984a.e, γ-ray emission time of flight=490.5s
time of max NM T NM = 06:52:30 UT
corresponds to Ep=500 MeV,
than time delay T NM relative γ-ray emission maximum
Tγ=06:46:30 UT is equal to 360 s .
In this case
proton time of flight is Tflight=(490+360) s.
Vp (500 MeV)=0.76c.

In this case proton path L= Tflight *Vp=1.32R and time difference
between 5 GeV and 500 MeV protons onset time has to be 195 s.

This value correspond l to NM rise time duration..
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