Exploring The Hard State Of Black Hole XRB's Through GRMHD Simulations
Abstract
We present two-dimensional numerical simulations of black hole accretion disks using a general relativistic magnetohydrodynamic (GRMHD) code that includes total energy conservation and is divergence free. The accretion disks are allowed to radiatively cool through a function that approximates bremsstrahlung, synchrotron, and Compton emissions. We focus our study particularly on parameters appropriate for stellar mass black holes in X-ray binaries. The simulations are most applicable to the Hard state of such systems. The main parameter we explore is the mass accretion rate, beginning several orders of magnitude below the Eddington limit, and gradually increasing until we reach the optically thick limit, where our simulations are no longer valid. Some attention is paid to comparing our simulation results to the predictions of the magnetically-dominated accretion flow (MDAF) model. If available, we may also show synthetic broadband spectra of these simulations.
- Publication:
-
American Astronomical Society Meeting Abstracts #215
- Pub Date:
- January 2010
- Bibcode:
- 2010AAS...21540403M