X-ray flare of CF Tuc (=HD 5303) (Kuerster+ 1996)

Details X-ray flare of CF Tuc (=HD 5303) (Kuerster+ 1996) X-ray flare of CF Tuc (=HD 5303) (Kuerster+ 1996)

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..33110211k&link_type=abstract

VizieR On-line Data Catalog: J/A+A/311/211. Originally published in: 1996A&A...311..211K

Computer Science

Stars: Flare

Scientific paper

Solar abundance fits to the quiescent spectra 1-3 and 20-35 were made with a two-component thermal plasma (model 1a) whereas sub-solar abundance fits to the quiescent spectra were made with a one-component thermal plasma (model 2a). Modifications of these models were used for the flare spectra 4-19 in order to account for the `quiescent background'. Thus solar abundance fits to the flare spectra were made with a thermal plasma of two variable components plus two components kept constant at the average quiescent values T_qu,cool=2.46*106K, EMqu,cool=0.49*1053cm-3, Tqu,hot=17.8* 106K, EMqu,hot=1.95*1053cm-3, and z=1.00 (model 1b). Sub-solar abundance fits to the flare spectra were made with a plasma of one variable component plus one component kept constant at the average quiescent values Tqu=13.0*106K, EMqu=5.20*1053cm-3, and z=0.10 (model 2b). In both cases the mean values of spectra 3, and 20-35 were used to account for the quiescent emission. (1 data file).

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