Mathematics – Logic
Scientific paper
Jun 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2703j&link_type=abstract
American Astronomical Society, SPD meeting #37, #27.03; Bulletin of the American Astronomical Society, Vol. 38, p.253
Mathematics
Logic
Scientific paper
: We present the observations and recently obtained results from the "Solar X-ray Spectrometer (SOXS)" mission, which was launched onboard GSAT-2 Indian spacecraft on 08 May 2003 to study the solar flares. The solid state detectors viz. Si PIN and Cadmium-Zinc-Telluride (CZT) were employed that operate at near room temperature. The Si PIN provides sub-keV energy resolution throughout its dynamic range of 4-25 keV. We present the X-ray emission characteristics of Fe and Fe/Ni line features found from the study of 10 M-class flares observed by SOXS mission. We also detected a new strong emission line peaking around 4.9 keV, supposed to be an ionic excitation from Ca. whcih may attract many atomic theoreticians and high energy astrophysicists. We present the measurement of peak energy (Ep) and equivalent width (w) of Fe and Fe/Ni-line features that varies as a function of temperature. We found that the equivalent width (w) of Fe-line feature increases exponentially with temperature up to 25 MK but later it increases very slowly up to 35 Mk and then it remains uniform up to 40 MK from where a downward trend is seen with higher temperature. We compare measurements of w of Fe line feature with calculations made earlier by various investigators and propose that these measurements may improve theoretical models. On the other hand w of Fe/Ni-line and newly detected Ca line features continuously increase with temperature until 54 MK. We interpret the variation of both Ep and w with temperature as the changes in the ionization and recombination conditions in the plasma during the flare interval and as a consequence the contribution from different ionic emission lines also varies. Our new findings may help in solving the paradigm of elemental abundances in solar standard model that emerged recently after precise helioseismological measurements.
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