Hydrodynamics and Radiation Transport in Radiation Dominated Accretion onto Neutron Stars

Details Hydrodynamics and Radiation Transport in Radiation Dominated Accretion onto Neutron Stars Hydrodynamics and Radiation Transport in Radiation Dominated Accretion onto Neutron Stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21721506w&link_type=abstract

American Astronomical Society, AAS Meeting #217, #215.06; Bulletin of the American Astronomical Society, Vol. 43, 2011

Physics

Scientific paper

The problem of spectral formation in accretion-powered X-ray pulsars was solved for the first time using an analytical model based on the fundamental physics in 2007, and the resulting spectra were shown to agree rather closely with those observed from several of the most luminous sources. However, in order to derive the analytical solutions, simplifying assumptions were made regarding the inflow velocity profile, the thermal structure of the plasma, the boundary conditions, and the geometry of the column. In this paper, the problem is revisited using a new numerical approach that facilitates the solution of a more realistic, coupled radiative-hydrodynamical model. The new model utilizes a conical geometry for the accretion flow and applies a robust free-streaming boundary condition at the top of the column, along with a "mirror" boundary condition at the neutron star surface. The temperature of the electrons is computed based on inverse-Compton equilibration, and the hydrodynamical structure of the column is determined by solving the coupled set of conservation equations for momentum, energy, and mass. The column-integrated spectra computed using the new model are compared with the data for several sources, and the resulting source parameters are compared with those computed using the original analytical model.

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