Synchrotron Radiation From Radiatively Inefficient Accretion Flow Simulations: Applications to Sgr A*

Details Synchrotron Radiation From Radiatively Inefficient Accretion Flow Simulations: Applications to Sgr A* Synchrotron Radiation From Radiatively Inefficient Accretion Flow Simulations: Applications to Sgr A*

2004-11-23

arxiv.org/abs/astro-ph/0411627v1

Astrophys.J. 621 (2005) 785-792

Astronomy and Astrophysics

Astrophysics

Accepted for publication in ApJ

Scientific paper

10.1086/427741

We calculate synchrotron radiation in three-dimensional pseudo-Newtonian magnetohydrodynamic simulations of radiatively inefficient accretion flows. We show that the emission is highly variable at optically thin frequencies, with order of magnitude variability on time-scales as short as the orbital period near the last stable orbit; this emission is linearly polarized at the 20-50 % level due to the coherent toroidal magnetic field in the flow. At optically thick frequencies, both the variability amplitude and polarization fraction decrease significantly with decreasing photon frequency. We argue that these results are broadly consistent with the observed properties of Sgr A* at the Galactic Center, including the rapid infrared flaring.

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