We analyze a Chandra HETGS observation of the single G-type giant HR 9024. The high flux allows us to examine spectral line and continuum diagnostics at high temporal resolution, to derive plasma parameters (thermal distribution, abundances, temperature,...). A time-dependent I D hydrodynamic loop model with semi-length 10(12) cm (similar to R-*), and impulsive footpoint heating triggering the flare, satisfactorily reproduces the observed evolution of temperature and emission measure, derived from the analysis of the strong continuum emission. The observed characteristics of the flare appear to be common features in very large flares in active stars (also pre-main sequence stars), possibly indicating some fundamental physics for these very dynamic and extreme phenomena in stellar coronae.
TESTA PAOLA, GARCIA-ALVAREZ DAVID, REALE F, HUENEMOERDER DAVID (2006). X-ray flare modeling in the single giant HR 9024. In ESA, Ed. by A. Wilson (pp.117-118).
X-ray flare modeling in the single giant HR 9024
TESTA, Paola;REALE, Fabio;
2006-01-01
Abstract
We analyze a Chandra HETGS observation of the single G-type giant HR 9024. The high flux allows us to examine spectral line and continuum diagnostics at high temporal resolution, to derive plasma parameters (thermal distribution, abundances, temperature,...). A time-dependent I D hydrodynamic loop model with semi-length 10(12) cm (similar to R-*), and impulsive footpoint heating triggering the flare, satisfactorily reproduces the observed evolution of temperature and emission measure, derived from the analysis of the strong continuum emission. The observed characteristics of the flare appear to be common features in very large flares in active stars (also pre-main sequence stars), possibly indicating some fundamental physics for these very dynamic and extreme phenomena in stellar coronae.
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