J/A+A/311/211ivo://CDS.VizieR/J/A+A/311/211doi:10.26093/cds/vizier.33110211CDSKuerster M.Schmitt J.H.M.M.1997-12-09T16:43:12Z1997-12-09T17:43:09ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frstellar-flaresSolar 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*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.1996A&A...311..211Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/311/211CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/311/211https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/311/211http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/311/211https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/311/211https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/311/211http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/311/211GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/311/211/table2Raymond-Smith model fits with solar and sub-solar metal abundances, z=1.0 and z=0.1.TTemperature, model 2 (3)1e+06Kphys.temperaturefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSqNumber of the spectrummeta.id;meta.mainintStateEmission state as inferred from the light curve (1)meta.codecharHJDHeliocentric Julian daydtime.epochdoubleNH1Hydrogen column density, model 1 (2)1e+19cm**-2phys.columnDensityfloate(NH1)uError in NH1, upper limit1e+19cm**-2stat.errorfloate(NH1)lError in NH1, lower limit1e+19cm**-2stat.errorfloatEMcoolEmission measure of the cooler plasma component, model 1 (2)1e+53cm**-3phys.emissMeasurefloate(EMcool)uError in EMcool, upper limit1e+53cm**-3stat.errorfloate(EMcool)lError in EMcool, lower limit1e+53cm**-3stat.errorfloatTcooltemperature of the cooler plasma component, model 1 (2)1e+06Kphys.temperaturefloate(Tcool)uError in Tcool, upper limit1e+06Kstat.errorfloate(Tcool)lError in Tcool, lower limit1e+06Kstat.errorfloatEMhotEmission measure of the hotter plasma component, model 1 (2)1e+53cm**-3phys.emissMeasurefloate(EMhot)uError in EMhot, upper limit1e+53cm**-3stat.errorfloate(EMhot)lError in EMhot, lower limit1e+53cm**-3stat.errorfloatThotTemperature of the hotter plasma component, model 1 (2)1e+06Kphys.temperaturefloate(Thot)uError in Thot, upper limit1e+06Kstat.errorfloate(Thot)lError in Thot, lower limit1e+06Kstat.errorfloatChi21Reduced chi-square of the fit, model 1 (2)stat.fit.paramfloatf_Chi21Number of degrees of freedom of chi2meta.code.errorintNH2Hydrogen column density, model 2 (3)1e+19cm**-2phys.columnDensityfloate(NH2)uError in NH2, upper limit1e+19cm**-3stat.errorfloate(NH2)lError in NH2, lower limit1e+19cm**-3stat.errorfloatEMEmission measure, model 2 (3)1e+53cm**-3phys.emissMeasurefloate(EM)uError in EM, upper limit1e+53cm**-3stat.errorfloate(EM)lError in EM, lower limit1e+53cm**-3stat.errorfloate(T)uError in T, upper limit1e+06Kstat.errorfloate(T)lError in T, lower limit1e+06Kstat.errorfloatChi22Reduced chi-square of the fit, model 2 (3)stat.fit.paramfloatf_Chi22Number of degrees of freedommeta.code.errorint