The aim of the work: Why the flare emission in cool chomospheric lines (H, Ca lines)
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M1.0 flare of 22 Oct 2002 RHESSI observations of the M 1.0 solar flare on 22 October 2002 A. Berlicki 1,2 , B. Schmieder 1 , N. Vilmer 1 , G. Aulanier 1 1) Observatoire de Paris, Section de Meudon, LESIA, FRANCE 2) Astronomical Institute of the Wrocław University, POLAND
description
RHESSI observations of the M 1.0 solar flare on 22 October 2002 A. Berlicki 1,2 , B. Schmieder 1 , N. Vilmer 1 , G. Aulanier 1 1) Observatoire de Paris, Section de Meudon, LESIA, FRANCE 2) Astronomical Institute of the Wroc ł aw University, POLAND. The aim of the work: - PowerPoint PPT Presentation
Transcript of The aim of the work: Why the flare emission in cool chomospheric lines (H, Ca lines)
M1.0 flare of 22 Oct 2002
RHESSI observations of the M 1.0solar flare on 22 October 2002
A. Berlicki 1,2, B. Schmieder 1, N. Vilmer 1, G. Aulanier 1
1) Observatoire de Paris, Section de Meudon, LESIA, FRANCE2) Astronomical Institute of the Wrocław University, POLAND
M1.0 flare of 22 Oct 2002
The aim of the work:
Why the flare emission in cool chomospheric lines (H, Ca lines) is observed for a long time during the late phase of solar flares ?
What kind of heating mechanism is effective during thegradual phase of solar flares ?
* Small flux of non-thermal electrons ? * Thermal conduction ? * Radiative heating by soft X-rays ?
We try to explain if the non-thermal component in X-ray emissioncould be present during the gradual phase of solar flares.
M1.0 flare of 22 Oct 2002
MDI - cont.
BBSO - H-alpha
M1.0 flare of 22 Oct 2002
IICONTCONT ( (Na D1,Na D1,THEMIS)THEMIS)
BBLONGLONG (NaD1, THEMIS) (NaD1, THEMIS)
HXR (RHESSI)HXR (RHESSI)
22 oct 2002
TRACE 195 ang.TRACE 195 ang.
HH flare (VTT) + flare (VTT) + RHESSIRHESSI
M1.0 flare of 22 Oct 2002
M1.0 flare of 22 Oct 2002
Thermal + non-thermal + Fe/Ni line complex (6.7 & 8 keV)
M1.0 flare of 22 Oct 2002
M1.0 flare of 22 Oct 2002
Thermal and non-thermal component during the gradual phase
a) Thermal energy of plasma:
b) Energy contained in the non-thermal electrons (thin target model): (Hudson et al. 1978, Sol. Phys. 60, 137)
(for ECUT-OFF = 10 keV)
- power-law indexB(x,y) – beta function10 – X-ray flux at 10 keV [photons cm-2 s-1 keV-1]
M1.0 flare of 22 Oct 2002
Thermal Eth and non-thermal Enth energy contained in the flare of October 22, 2002.
? ? ?
M1.0 flare of 22 Oct 2002
Conclusions:
1) During the analysed period the thermal energy is dominant,
2) Non-thermal component provide a marginal input to the total energy but it is necessary to explain the spectra between 10 and 20 keV,
? ? ?
* Thin or thick target,
* Distinguish between thermal and non-thermal emission at low energies,
* Relation between Ecut-off and the energy contained in non-thermal electrons – very sensitive !
