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

20-25 keV60-150 keV

03 novembre 2003

From Liu et al, 2004

2 parts for the non-thermal emission

FP sources at 60-150 keVLT at 20-25 keV

3 November 2003 event

Liu et al, 2004

Foot point separationincreases between first and second peak

Loop top source risesin the corona betweenfirst and second peak

X-rays

radio

Phoenix

OSRA

Wind/waves

Type II

Type III like

Large band continuum Enhancement and modulations (radio and X-rays)

Also a fast CMESeen 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

X-rays

Mm/cmBern obs

Dm/mNRH

Type IIIType II

Details of the modulations

Broad-band modulations

Combined radio spectrum1 first part2 before modulations3 four modulations to 09:59:50 UT4 fifth modulation from 10:00:00 UTAdjustment between NRH and RSTN at 410 MHzNo adjustement with Bern

Radio spectrum:Combination of plasma emissionsand of gyrosynchrotron emissions

plasma

gyrosynchrotron

From 09:56:30 continuous rise of theRadio spectrum from 400 MHz to several 10 GHz

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 linesIn part 1

Part 2: 2.2 MeV line

Look at the continuumSearch forFlattening at high energies

Link between HXR/GR and cm/mm emitting electrons

Note the flattening ofthe photon spectrum above400 keV-600 keVSpectral index:-2.1 and -1.6

HXR/GR spectra

More details…• 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 keV2 keV to 100 keV5 keV to 150 keV10 keV to 200 keV20 keV to 300 keV50 keV to 600 keV100 keV to 1000 keV200 keV to 1600 keV300 keV to 2500 keV500 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= -2.12= 0.7

We marginally see the 2.2 MeV line. There is a good consistency with the parameters obtained with binning 12With 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= -1.62= 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

peakThe 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= -1.562= 2.32Only the 2.2 MeV line is seenThe results are consistent with the ones of binning 12

Add the 2.2 MeV lineOther lines?

Simple relationship between the spectral indexes of cm-mm and HXR/GR producing electrons

1.22 0.9r

X-ray emission (thick targetFrom precipitating electrons

Microwave from trapped 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: =1.22-0.9with 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 eventThe predicted spectral index ofGyrosynchrotron emissions would be-1.6 to -1.12 if emitted by the hardestpart of the electron population

Seems too steep…What about numbers?