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
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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)
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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.