Constraining the Accretion Flow in Sgr A* by General Relativistic Dynamical and Polarized Radiative Modeling
arXiv:1212.4149 · doi:10.1017/S1743921312020157
Abstract
We briefly summarize the method of simulating Sgr A* polarized sub-mm spectra from the accretion flow and fitting the observed spectrum. The dynamical flow model is based on three-dimensional general relativistic magneto hydrodynamic simulations. Fully self-consistent radiative transfer of polarized cyclo-synchrotron emission is performed. We compile a mean sub-mm spectrum of Sgr A* and fit it with the mean simulated spectra. We estimate the ranges of inclination angle theta=42-75deg, mass accretion rate Mdot=(1.4-7.0)*10^{-8}Msun/yr, and electron temperature Te=(3-4)*10^{10}K at 6M. We discuss multiple caveats in dynamical modeling, which must be resolved to make further progress.
2 pages, no figures, for Proceedings of IAU Symposium 290 "Feeding compact objects: Accretion on all scales", eds C.M. Zhang, T. Belloni, M. Mendez & S.N. Zhang
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