J/A+A/386/1001ivo://CDS.VizieR/J/A+A/386/1001doi:10.26093/cds/vizier.33861001CDSGaensickeB.T.BrajeT.M.RomaniR.W.2002-07-20T20:50:34Z2002-07-20T20:50:07ZCDS support team

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

cds-question@unistra.frastronomical-modelsstellar-atmospheresWe present a new grid of LTE model atmospheres for weakly magnetic (B<~10^10^G) neutron stars, using X opacity and equation of state data from the OPAL project and employing a fully frequency- and angle-dependent radiation transfer. Model spectra for low-field neutron stars with three different photospheric compositions are presented: (1) pure hydrogen atmospheres, (2) atmospheres with solar abundances, and (3) pure iron atmospheres. Each grid covers 29 effective temperatures log(Teff[K])=5.10-6.50 in steps of 0.05. The model spectra are tabulated as angle-averaged unredshifted (surface) Eddington fluxes. All spectra have been calculated for a canonical neutron star configuration, M_ns_=1.4M_{sun}_, R_ns_=10km, corresponding to a surface gravitational acceleration of log(g)=14.386. The same model grids are also available as XSPEC tables at http://legacy.gsfc.nasa.gov/docs/xanadu/xspec/models/gbr.html2002A&A...386.1001Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/386/1001CatalogResearchIsServedByTAP VizieR generic servicerelated-tohttp://legacy.gsfc.nasa.gov/docs/xanadu/xspec/models/gbr.html :https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/386/1001https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/386/1001http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/386/1001https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/386/1001https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/386/1001http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/386/1001GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/386/1001/hNeutron star model spectra, pure hydrogen atmosphererecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEEnergy levelkeVem.energydoubleHe5.10Eddington flux for log(Teff)=5.10 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.15Eddington flux for log(Teff)=5.15 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.20Eddington flux for log(Teff)=5.20 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.25Eddington flux for log(Teff)=5.25 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.30Eddington flux for log(Teff)=5.30 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.35Eddington flux for log(Teff)=5.35 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.40Eddington flux for log(Teff)=5.40 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.45Eddington flux for log(Teff)=5.45 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.50Eddington flux for log(Teff)=5.50 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.55Eddington flux for log(Teff)=5.55 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.60Eddington flux for log(Teff)=5.60 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.65Eddington flux for log(Teff)=5.65 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.70Eddington flux for log(Teff)=5.70 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.75Eddington flux for log(Teff)=5.75 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.80Eddington flux for log(Teff)=5.80 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.85Eddington flux for log(Teff)=5.85 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.90Eddington flux for log(Teff)=5.90 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.95Eddington flux for log(Teff)=5.95 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.00Eddington flux for log(Teff)=6.00 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.05Eddington flux for log(Teff)=6.05 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.10Eddington flux for log(Teff)=6.10 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.15Eddington flux for log(Teff)=6.15 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.20Eddington flux for log(Teff)=6.20 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.25Eddington flux for log(Teff)=6.25 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.30Eddington flux for log(Teff)=6.30 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.35Eddington flux for log(Teff)=6.35 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.40Eddington flux for log(Teff)=6.40 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.45Eddington flux for log(Teff)=6.45 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.50Eddington flux for log(Teff)=6.50 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleJ/A+A/386/1001/feNeutron star model spectra, pure iron atmosphererecnoRecord number assigned by the VizieR team. 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Should Not be used for identification.meta.recordintEEnergy levelkeVem.energydoubleHe5.10Eddington flux for log(Teff)=5.10 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.15Eddington flux for log(Teff)=5.15 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.20Eddington flux for log(Teff)=5.20 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.25Eddington flux for log(Teff)=5.25 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.30Eddington flux for log(Teff)=5.30 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.35Eddington flux for log(Teff)=5.35 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.40Eddington flux for log(Teff)=5.40 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.45Eddington flux for log(Teff)=5.45 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.50Eddington flux for log(Teff)=5.50 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.55Eddington flux for log(Teff)=5.55 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.60Eddington flux for log(Teff)=5.60 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.65Eddington flux for log(Teff)=5.65 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.70Eddington flux for log(Teff)=5.70 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.75Eddington flux for log(Teff)=5.75 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.80Eddington flux for log(Teff)=5.80 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.85Eddington flux for log(Teff)=5.85 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.90Eddington flux for log(Teff)=5.90 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe5.95Eddington flux for log(Teff)=5.95 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.00Eddington flux for log(Teff)=6.00 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.05Eddington flux for log(Teff)=6.05 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.10Eddington flux for log(Teff)=6.10 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.15Eddington flux for log(Teff)=6.15 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.20Eddington flux for log(Teff)=6.20 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.25Eddington flux for log(Teff)=6.25 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.30Eddington flux for log(Teff)=6.30 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.35Eddington flux for log(Teff)=6.35 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.40Eddington flux for log(Teff)=6.40 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.45Eddington flux for log(Teff)=6.45 (1)mW.m**-2.keV**-1phot.flux;em.X-raydoubleHe6.50Eddington flux for log(Teff)=6.50 (1)mW.m**-2.keV**-1phot.flux;em.X-raydouble