Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002esasp.506..549b&link_type=abstract
In: Solar variability: from core to outer frontiers. The 10th European Solar Physics Meeting, 9 - 14 September 2002, Prague, Cze
Physics
Solar Chromosphere: Heating, Solar Flares
Scientific paper
In this paper we present the analysis of energetics of solar flaring chromosphere heated by soft X-ray radiation coming from overlying hot flare loops. During the solar flare, a large amount of its energy is emitted from hot coronal part in soft X-ray spectral range. This radiation can penetrate into the chromosphere and transmit the energy. This additional heating modifies vertical structure of the chromosphere and it can cause the enhanced emission from some parts of the flare. Therefore, such a mechanism can be responsible for emission of chromospheric flaring structures commonly observed in Hα and other spectral lines during the gradual phases when non-thermal processes are unimportant. To analyze the effect of X-ray heating we used the observations of the solar flare of 25 September 1997. This flare was observed with the Wroclaw Multichannel Subtractive Double Pass spectrograph (MSDP) coupled with the Large Coronagraph. We also use X-ray observations of the flare taken with the SXT telescope. Within the approximation of the quasi steady-state we have calculated the deposit of X-ray energy in the chromosphere. By means of the non-LTE radiative transfer calculations we show that enhanced emission of some H-alpha structures observed during the gradual phase of this solar flare can be partially explained in terms of the soft X-ray heating of the chromosphere by hot 'post-flare' loops seen on the SXT images. We also analyzed the energy budget of X-ray heated flaring chromosphere and found that radiative losses from the chromosphere can be balanced by soft X-ray heating only in some layers of the solar chromosphere.
Berlicki Arkadiusz
Heinzel Petr
Jakimiec Jerzy
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