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Constraining the Accretion Flow in Sgr A* by General Relativistic Dynamical and Polarized Radiative Modeling

Published online by Cambridge University Press:  21 February 2013

Roman V. Shcherbakov ,
Robert F. Penna  and
Jonathan C. McKinney
Roman V. Shcherbakov
Affiliation:
Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA email: roman@astro.umd.edu Hubble Fellow
Robert F. Penna
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
Jonathan C. McKinney
Affiliation:
Physics Department, University of Maryland, College Park, MD 20742-4111, USA
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Abstract

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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 θ=42°–75°, mass accretion rate Ṁ=(1.4-7.0)×10−8M⊙year−1, and electron temperature Te=(3–4)×1010K at 6M. We discuss multiple caveats in dynamical modeling, which must be resolved to make further progress.

Keywords

accretionaccretion disksblack hole physicsGalaxy: centerradiative transferrelativistic processespolarization
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S290: Feeding Compact Objects: Accretion on All Scales , August 2012 , pp. 309 - 310
Copyright
Copyright © International Astronomical Union 2013

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