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

06:35 06:40 06:45 06:50 06:55 07:00100

101

102

103

104

105

C

ou

nts

s -1

UT, hh:mm

Proton onset

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

2000

4000

6000

0

400

800

1200

0

20

40

60

0

2

4

0,0

0,2

0,4

06:43 06:44 06:45 06:46 06:47 06:48 06:49

0,00

0,04

0,08

0,00

0,01

0,02

0,00

0,01

0,000

0,005

0,010

0,000

0,003

0,006

0,000

0,001

06:43 06:44 06:45 06:46 06:47 06:48 06:49

0,0000

0,0001

UT, hh:mm

0.082-0.23 MeV

F, c

m -2

s -1 M

eV -1

0.23-0.78 MeV

0.78 -2 MeV

2-6.2 MeV

6.2-10.8 MeV

10.8-23.2 MeV

23.2 -40.3 MeV

40.3-63 MeV

XG10 15 point AA Smoothing of RFLUX565_XG10

63-93 MeV

93-155 MeV

0.043-0.082 MeV

XG12 15 point AA Smoothing of RFLUX565_XG12

UT, hh:mm

155-310 MeV

Energy spectra in the phases IA and IB

0,01 0,1 1 10 10010-5

10-3

10-1

101

103

SPRN

IAIB

SONG

20 January, 2005

F,

sm -2

s -1

Me

V -1

E, MeV

Distinct 0 component is seen in the phase IB.

The absolute flux is compared with that of SPRN- X-ray detector onboard CORONAS

10-2 100 102

1x10-4

10-2

100

102

104

10-2 100 102 10-2 100 102

1x10-4

10-2

100

102

104

F,

cm

-2 s

-1 M

eV-1

IA

E, MeV

IB

Int-II?

Comparison of RHESSI and SPRN time profiles in similar energy windows.

06:40 06:45 06:50 06:55 07:000

20000

40000

60000 SXR component substructed

F, c

m-2 s

-1 M

eV -1

UT, hh:mm

48-120 keV

0

1000

2000 RHESSI 50-100 keV

SPRN

18<Ex<48 keV4000

8000

0

4000

8000

06:40 06:43 06:46 06:48 06:510

1000

2000

3000

Co

un

ts s

-1

UT

HESSI 100 keVSONG 82 keV

0

500

1000

F, s

m-2 s

-1 M

eV

-1

06:40 06:43 06:46 06:48 06:51

6

8

10

Co

un

ts s

-1

F c

m -2

s -1

Me

V -1

UT, hh:mm

HESSI 7 MeVSONG 6.2-10.8 MeV

0,00

0,02

0,04

0,06

0,08

0,10

06:40 06:43 06:46 06:48 06:51

80

100

120

140

160

180

Co

un

ts s

-1

UT, hh:mm

F,

sm -2

s-1 M

eV

-1

HESSI 800 keVSONG 775 KeV

0

2

4

06:40 06:43 06:46 06:48 06:51

100

200

300

Co

un

ts s

-1

F, c

m -2

s-1 M

eV

-1

X Axis Title

HESSI 300 keVSONG 230 keV

0

20

40

60

06:43 06:46 06:48 06:51 06:54 06:57

0,0

0,4

0,8

1,2

1,6

RHESSI

UT, hh:mm

0

20

40

60

80

SONG LINE 2.2 MeV

January 20,2005

Arb

itra

ry U

nits

06:40 06:42 06:44 06:46 06:48 06:50 06:52 06:54-5

0

5

10

15

20

E >60 MeV E 0.78-2 MeV

Cou

nts

s -1

Cou

nts

s -1

UT, hh:mm

0,0

0,5

1,0

line 511 keV RHESSI

Arb

itra

ry u

nits

0

20

40

60

80

What we see at the end of the phase IB

06:44 06:45 06:46 06:47 06:48 06:49 06:50 06:51

100

Cou

nt s

-1

Cou

nt s

-1

UT, hh:mm

10

5 points sm 6.2-10.8 MeV

5 points sm 41-300 MeV

Decay of bremmstrahlung emission becomes more steep than

that of 0 emission. It seems that variation of the intensities becomes asynchronious.

06:44 06:45 06:46 06:47 06:48 06:49 06:50 06:512000

3000

4000

5000

6000

Nobeyama

F,s

fu

Ut, hh:mm

2GHz

Plasma temperature begins to decrease at the end of the phase IB

0

10

20

30IIIBIA E>60 МэВ

Отсчёты, с-1

UT, час : мин

06:40 06:42 06:44 06:46 06:48 06:50 06:52 06:54 06:560

4000

8000E 0.23-0.78 МэВ

110

1001000

% South Pole NM

0

10

20

30IIIBIA E>60 МэВ

Отсчёты, с-1

UT, час : мин

06:40 06:42 06:44 06:46 06:48 06:50 06:52 06:54 06:560

4000

8000E 0.23-0.78 МэВ

110

1001000

% South Pole NM

If the L>L1 than escaping time shifted to more earlier time.

????

The shortest path of protons L1 =1.055RTime 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

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..