3 November 2003 event
HXR/Gamma-ray and radio
observations
Rhessi_workshop
3 November 2003 event
-GOES X 3.9 (AR 0488)
-Observed in X-rays (keV-a few MeV
(RHESSI)
(Liu, Jiang, Liu et al, 2004; Veronig,
Karlicky, Vrsnak et al. 2005)
-Observed at m/dm wavelengths by the
Nançay Radioheliograph
(150 MHz-450 MHz) and at cm/mm
wavelengths by Bern (16 GHz-89
GHz) and by RSTN
(Dauphin, Vilmer, Lüthi et al, 2005)
(Dauphin, Vilmer, Krucker, 2006)
3 November 2003 event
60-150 keV
20-25 keV
From Liu et al, 2004
2 parts for the non-thermal emission
FP sources at 60-150 keV
LT at 20-25 keV
03 novembre 2003
3 November 2003 event
Foot point separation
increases between first
and second peak
Loop top source rises
in the corona between
first and second peak
Liu et al, 2004
X-rays
Type II
Phoenix
radio
Type III like OSRA
Wind/waves
Large band continuum
Enhancement and modulations
(radio and X-rays)
Also a fast CME
Seen by Lasco
3 November 2003 event
- Broad band modulations at X-ray and mm-cm to
dm wavelengths: origin?
- Rising soft X-ray loop and CME?
- Rising X-ray loop and type II onset at high
frequencies
- Link between HXR/GR emitting electrons and
mm/cm emitting electrons
Broad-band modulations
X-rays
Mm/cm
Bern obs
Type II
Type III
Dm/m
NRH
Details of the modulations
Radio spectrum:
Combination of plasma emissions
and of gyrosynchrotron emissions
plasma
From 09:56:30 continuous rise of the
Radio spectrum from 400 MHz to several 10 GHz
gyrosynchrotron
Combined radio spectrum
1 first part
2 before modulations
3 four modulations to 09:59:50 UT
4 fifth modulation from 10:00:00 UT
Adjustment between NRH and RSTN at
410 MHz
No adjustement with Bern
Origin of dm/m radio continua??:
Gyrosynchrotron emission of a few MeV electrons
(Boischot/Denisse 1957)
Plasma emissions (Duncan, 1981; Trottet et al,1981)
Here: gyrosynchrotron emission:
3 November 2003
No evidence of lines
In part 1
Part 2: 2.2 MeV line
Look at the continuum
Search for
Flattening at high energies
Link between HXR/GR and cm/mm emitting electrons
Note the flattening of
the photon spectrum above
400 keV-600 keV
Spectral index:-2.1 and -1.6
HXR/GR spectra
More details…
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We first look at rear detectors and we started to bin with binning 12:
Detectors 2 and 7 excluded (no pulse pile up correction)
1 keV width 3 to 60 keV
2 keV
to 120 keV
5 keV
to 250 keV
10 keV to 2250 keV
50 keV 2250 to 7200 keV
200 keV 7.2 MeV to 17 MeV
+ special binning around 511 keV and 2.2 MeV
Results:
Interval 1 : 094901-094957 UT
A@50 keV=8.25
1= -3.4 Eb= 396 keV 2= -2.2
2= 0.85
We also note the presence of a 511kev and a 2.2 MeV line
Same analysis with a different binning: binning 13 with larger energy bins
since we are not really interested by lines
Binning 13:
129 channels:
1 kev width to 3 keV
2 keV to 100 keV
5 keV to 150 keV
10 keV to 200 keV
20 keV to 300 keV
50 keV to 600 keV
100 keV to 1000 keV
200 keV to 1600 keV
300 keV to 2500 keV
500 keV to…
+ 20 keV channel around 511 keV
+50 keV channel around 2.2 MeV
Results:
Interval 1 : 094902-095002 UT
A@50 keV=7.19
1= -3.3 Eb= 408 keV 2= -2.1
2= 0.7
We marginally see the 2.2 MeV line. There is a good consistency with the parameters obtained with
binning 12
With this binning, we better see that the signal is above the background .
Interval2:
Results:
Interval 2 : 095850-100130 UT
A@50 keV=3.5
1= -3.2
Eb= 597 keV 2= -1.6
2= 1.09
We also see the 511 keV? and
2.2 MeV lines
The spectrum flattens at low
energies below 200 kev (the fit
is done above 180 keV) .
The slope is similar between
200 keV and the break energy
is larger compared to the first
peak
The slope is flatter above the
break than in the first peak.
The signal is a bit above the
background
With Binning 13:
Results:
Interval 2 : 095850-100130
UT
A@50 keV=3.1
1= -3.18 Eb= 619 keV
2= -1.56
2= 2.32
Only the 2.2 MeV line is
seen
The results are consistent
with the ones of binning 12
Add the 2.2 MeV line
Other lines?
Simple relationship between the spectral indexes
of cm-mm and HXR/GR producing electrons
Microwave from trapped
electrons
  1.22  0.9r
X-ray emission (thick target
From precipitating electrons
If HXR photon spectral index: 
Thick-target emitting electrons : precipitating flux F: X=  +1
Relationship between F and N in the loop: F=N  ( time spent in the loop)
If free streaming of relativistic electrons or turbulent trapping:   E0
: index of microwave radiation: =1.22-0.9
with  spectral index of electrons in the loop
Link between HXR/GR and cm/mm emitting
electrons
Note the flat spectrum between 50 and 89 GHz
What is the relationship between
HXR/GR and cm/mm emitting
Electrons??
3 November event
The predicted spectral index of
Gyrosynchrotron emissions would be
-1.6 to -1.12 if emitted by the hardest
part of the electron population
Seems too steep…
What about numbers?