Steady models of optically thin, magnetically supported two-temperature accretion disks around a black hole

Details Steady models of optically thin, magnetically supported two-temperature accretion disks around a black hole Steady models of optically thin, magnetically supported two-temperature accretion disks around a black hole

Apr 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..238..421o&link_type=abstract

Black Holes from Stars to Galaxies -- Across the Range of Masses. Edited by V. Karas and G. Matt. Proceedings of IAU Symposium #

Computer Science

Scientific paper

We obtained steady solutions of optically thin two-temperature accretion disks around black hole taking into account the magnetic pressure and magnetic tension force. General relativistic effects are simulated by using the pseudo-Newtonian potential. We included relativistic bremsstrahlung cooling, synchrotron cooling and inverse Compton effects. We adopted α-prescription of viscosity and assumed that the disk is threaded by toroidal magnetic field. We found that when the surface density of the optically thin disk exceeds a critical value, magnetic pressure dominated new branch appears in the thermal equilibrium curves, on which the radiative cooling is efficient. We call this branch `low-β branch'. As a consequence, thermal equilibrium curves show `Z'-shape in the plane of surface density and temperature, or mass accretion rate. This indicate that as the mass accretion rate increases, an optically thin hot accretion disk makes transition to a magnetic pressure dominated, optically thin cool disk. This disk corresponds to the X-ray hard, luminous disk observed during the transition from a low/hard state to a high/soft state in black hole candidates. We also obtained global steady transonic solutions including such transition layer.

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