General Relativistic Radiative Transfer in Hot Astrophysical Plasmas: a Characteristic Approach

In this paper we present a characteristic method for solving the transfer equation in differentially moving media in a curved spacetime. The method is completely general, but its capabilities are exploited at best in presence of symmetries, when the existence of conserved quantities allows to derive analytical expressions for the photon trajectories in phase space. In spherically–symmetric, stationary configurations the solution of the transfer problem is reduced to the integration of a single ordinary differential equation along the bi–parametric family of characteristic rays. Accurate expressions for the radiative processes relevant to continuum transfer in a hot astrophysical plasma have been used in evaluating the source term, including relativistic e–p, e–e bremsstrahlung and Compton scattering. A numerical code for the solution of the transfer problem in moving media in a Schwarzschild spacetime has been developed and tested. Some applications, concerning “hot” and “cold” accretion onto non–rotating black holes as well as static atmospheres around neutron stars, are presented and discussed. Subject headings: accretion, accretion disks – numerical methods – radiative transfer – relativity