Accretion Models for Sgr A*

Eliot Quataert1

1UC Berkeley, Astronomy Department, 601 Campbell Hall, Berkeley, CA 94720

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I describe radiatively inefficient accretion flow models for Sgr A*. Recent theoretical arguments strongly favor an accretion rate onto Sgr A* that is much less than the canonical Bondi rate. I review these results, emphasizing progress in understanding the MHD and kinetic physics that governs the accretion flow dynamics. I then discuss the interpretation of radio and X-ray observations of Sgr A* in the context of radiatively inefficient accretion flow models.