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

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*10^6K, EM_qu,cool=0.49*10^53cm^-3, T_qu,hot =17.8*10^6K, EM_qu,hot=1.95*10^53cm^-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 T_qu=13.0*10^6K, EM_qu=5.20*10^53cm^-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.