J/A+A/581/A83ivo://CDS.VizieR/J/A+A/581/A83doi:10.26093/cds/vizier.35810083CDSNattila J.Suleimanov V.F.Kajava J.J.EPoutanen J.2015-09-08T07:58:14Z2015-09-08T07:56:32ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmospheresx-ray-binary-starsLow-mass X-ray binaries hosting neutron stars (NS) exhibit thermonuclear (type-I) X-ray bursts, which are powered by unstable nuclear burning of helium and/or hydrogen into heavier elements deep in the NS "ocean". In some cases the burning ashes may rise from the burning depths up to the NS photosphere by convection, leading to the appearance of the metal absorption edges in the spectra, which then force the emergent X-ray burst spectra to shift toward lower energies. These effects may have a substantial impact on the color correction factor fc and the dilution factor w, the parameters of the diluted blackbody model F_E_=wB_E_(f_c_T_eff_) that is commonly used to describe the emergent spectra from NSs. The aim of this paper is to quantify how much the metal enrichment can change these factors. We have developed a new NS atmosphere modeling code, which has a few important improvements compared to our previous code required by inclusion of the metals. The opacities and the internal partition functions (used in the ionization fraction calculations) are now taken into account for all atomic species. In addition, the code is now parallelized to counter the increased computational load.2015A&A...581A..83Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/581/A83CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/527/A139 : Xray bursting neutron star atmos. models (Suleimanov+, 2011)J/A+A/545/A120 : Xray bursting neutron star atmos. models II (Suleimanov+ 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/581/A83https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/581/A83http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/581/A83https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/581/A83https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/581/A83http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/581/A83GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/581/A83/setAtmosphere parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSet[1/12] Set numbermeta.id;meta.mainintXX abundance (0.738, 0.550, 0.352, 0.0)phys.abund.XfloatYY abundance (0.249, 0.185, 0.118, 0.0)phys.abund.YfloatZZ abundance (0.013, 0.265, 0.530, 1.0)src.redshiftfloatloggLogarithm of surface gravity (14.0, 14.3, 14.6)log(cm.s**-2)phys.gravityfloatTEddEddington temperature (12 values)keVphys.temperature.effectivefloatRNeutron star radius (8.16, 10.88, 14.80)kmphys.size.radiusfloatzRedshift (0.18, 0.27, 0.42)src.redshiftfloatLumNumber of luminosities for a given setstat.fit.paramintJ/A+A/581/A83/tablebColor correction and dilution factorsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSet[1/12] Set numbermeta.id;meta.mainintlRelative luminosity L/L_Edd (1)phys.luminosity;arith.ratiofloatgrad/gRatio of the radiation acceleration to gravitystat.fit.paramfloatTeffEffective temperaturekeVphys.temperature.effectivefloatfc1Color correction factor f_c_ (2)arith.factor;phot.fluxfloatwDilution factor warith.factor;pos.distancefloatw*fc+4Product of dilution factor and (fc)^4^arith.factor;pos.distancefloat