Volume 527, March 2011
|Number of page(s)||12|
|Published online||11 February 2011|
X-ray bursting neutron star atmosphere models: spectra and color corrections⋆
Institute for Astronomy and Astrophysics, Kepler Center for Astro and
Particle Physics, Eberhard Karls University,
e-mail: email@example.com; firstname.lastname@example.org
2 Kazan Federal University, Kremlevskaja str. 18, Kazan 420008, Russia
3 Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu, Finland
Accepted: 17 December 2010
Aims. X-ray bursting neutron stars in low-mass X-ray binaries constitute an appropriate source class for constraining the masses and radii of neutron stars, but a sufficiently extended set of corresponding model atmospheres is necessary for these investigations.
Methods. We computed such a set of model atmospheres and emergent spectra in a plane-parallel, hydrostatic, and LTE approximation with Compton scattering taken into account.
Results. The models were calculated for six different chemical compositions: pure hydrogen, pure helium, and a solar mix of hydrogen and helium with various heavy element abundances Z = 1,0.3,0.1, and 0.01 Z⊙. For each chemical composition the models are computed for three values of surface gravity, log g =14.0, 14.3, and 14.6, and for 20 values of the luminosity in units of the Eddington luminosity, L/LEdd, in the range 0.001–0.98. The emergent spectra of all models are redshifted and fitted by a diluted blackbody in the RXTE/PCA 3–20 keV energy band, and corresponding values of the color correction (hardness factors) fc are presented.
Conclusions. Theoretical dependences fc–L/LEdd can be fitted to the observed dependence K −1/4–F of the blackbody normalization K on flux during cooling stages of X-ray bursts to determine the Eddington flux and the ratio of the apparent neutron star radius to the source distance. If the distance is known, these parameters can be transformed to the constraints on neutron star mass and radius. Theoretical atmosphere spectra can also be used for direct comparison with the observed X-ray burst spectra.
Key words: radiative transfer / scattering / methods: numerical / stars: neutron / stars: atmospheres / X-rays: stars
Tables A.1 and A.2 are only available in electronic form at CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/527/A139
© ESO, 2011
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