Volume 545, September 2012
|Number of page(s)||16|
|Published online||18 September 2012|
X-ray bursting neutron star atmosphere models using an exact relativistic kinetic equation for Compton scattering⋆,⋆⋆
Institut für Astronomie und Astrophysik, Kepler Center for Astro and
Particle Physics, Universität Tübingen,
e-mail: firstname.lastname@example.org; email@example.com
2 Kazan Federal University, Kremlevskaja str. 18, 420008 Kazan, Russia
3 Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu, Finland
Accepted: 13 July 2012
Context. Theoretical spectra of X-ray bursting neutron star (NS) model atmospheres are widely used to determine the basic NS parameters such as their masses and radii. Compton scattering, which plays an important role in spectra formation at high luminosities, is often accounted for using the differential Kompaneets operator, while in other models a more general, integral operator for the Compton scattering kernel is used.
Aims. We construct accurate NS atmosphere models using for the first time an exact treatment of Compton scattering via the integral relativistic kinetic equation. We also test various approximations to the Compton scattering redistribution function and compare the results with the previous calculations based on the Kompaneets operator.
Methods. We solve the radiation transfer equation together with the hydrostatic equilibrium equation accounting exactly for the radiation pressure by electron scattering. We use the exact relativistic angle-dependent redistribution function as well as its simple approximate representations.
Results. We thus construct a new set of plane-parallel atmosphere models in local thermodynamic equilibrium (LTE) for hot NSs. The models were computed for six chemical compositions (pure H, pure He, solar H/He mix with various heavy elements abundances Z = 1, 0.3, 0.1, and 0.01 Z⊙, and three surface gravities log g = 14.0, 14.3, and 14.6. For each chemical composition and surface gravity, we compute more than 26 model atmospheres with various luminosities relative to the Eddington luminosity LEdd computed for the Thomson cross-section. The maximum relative luminosities L/LEdd reach values of up to 1.1 for high gravity models. The emergent spectra of all models are redshifted and fitted by diluted blackbody spectra in the 3−20 keV energy range appropriate for the RXTE/PCA. We also compute the color correction factors fc.
Conclusions. The radiative acceleration grad in our luminous, hot-atmosphere models is significantly smaller than in corresponding models based on the Kompaneets operator, because of the Klein-Nishina reduction of the electron scattering cross-section, and therefore formally “super-Eddington” model atmospheres do exist. The differences between the new and old model atmospheres are small for L/LEdd < 0.8. For the same grad/g, the new fc are slightly larger (by approximately 1%) than the old values. We also find that the model atmospheres, the emergent spectra, and the color correction factor computed using angle-averaged and approximate Compton scattering kernels differ from the exact solutions by less than 2%.
Key words: radiative transfer / scattering / methods: numerical / stars: atmospheres / stars: neutron / X-rays: stars
Appendices are available in electronic form at http://www.aanda.org
Tables D.1–D.3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/545/A120
© ESO, 2012
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