J/ApJ/376/161ivo://CDS.VizieR/J/ApJ/376/161doi:10.26093/cds/vizier.13760161CDSMadej J.2018-02-01T11:50:43Z2014-12-01T09:09:31ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmospheresx-ray-binary-starsX-ray burst sources represent a class of accreting neutron stars in close binary systems which do not exhibit any traces of the magnetic field. We present new method of hot model atmosphere computations with account of Compton scattering on free electrons and computed set of plane-parallel hydrogen-helium atmospheres and X-ray spectra of bursting neutron stars. Models were computed with precise angle-dependent radiative transfer under constrains of radiative and hydrostatic equilibrium. Compton scattering opacity included both the Klein-Nishina corrections and the effects of relativistic Maxwellian thermal motion of scattering electrons. Compton redistribution function allows for large energy exchange between X-ray photons and scattering electrons.1991ApJ...376..161Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/376/161CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AcA/41/73 : Model atmospheres of X-ray bursting neutron stars (Madej, 1991)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/376/161https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/376/161http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/376/161https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/376/161https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/376/161http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/376/161GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/376/161/table1*Model parameters and f_c_=T_col_/T_eff_ ratios (spectral hardening factor)fc6[1.62/1.62]? Spectral hardening factor for logg6stat.paramfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintnr[1/4] Index of effective temperaturemeta.idintprimaryTeffCorresponding effective temperature (8.00E+06, 1.257E+07, 2.00E+07, 3.00E+07)Kphys.temperature.effectivedoublespPlot X-ray spectrum for this temperaturemeta.ref.urlcharloggcr[12.39/14.65] Logarithm of critical gravitylog(cm.s**-2)phys.gravityfloatlogg1[15] Logarithm of surface gravity 1log(cm.s**-2)phys.gravityfloatfc1[1.36/1.41] Spectral hardening factor for logg1stat.paramfloatlogg2[14.5/14.8] Logarithm of surface gravity 2log(cm.s**-2)phys.gravityfloatfc2[1.36/1.48] Spectral hardening factor for logg2stat.paramfloatlogg3[14.0/14.7] Logarithm of surface gravity 3log(cm.s**-2)phot.flux.density.sbfloatfc3[1.36/1.55] Spectral hardening factor for logg3stat.paramfloatlogg4[13.5/14.1]? Logarithm of surface gravity 4log(cm.s**-2)phys.gravityfloatnullablefc4[1.45/1.52]? Spectral hardening factor for logg4stat.paramfloatnullablelogg5[13.0/14.0]? Logarithm of surface gravity 5log(cm.s**-2)phys.gravityfloatnullablefc5[1.52/1.58]? Spectral hardening factor for logg5stat.paramfloatnullablelogg6[12.5/13.2]? Logarithm of surface gravity 6log(cm.s**-2)phys.gravityfloatnullableJ/ApJ/376/161/table2Photon energy and fluxesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintnr[1/4] Index of effective temperaturemeta.idintE[0.058/62.211] Photon energykeVem.energyfloatFE1? Log flux F_E_ for logg1log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullableFE2? Log flux F_E_ for logg2log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullableFE3? Log flux F_E_ for logg3log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullableFE4? Log flux F_E_ for logg4log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullableFE5? Log flux F_E_ for logg5log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullableFE6? Log flux F_E_ for logg6log(mW.m**-2.keV**-1)phot.flux;em.X-rayfloatnullable