What Is the Accretion Rate in Sagittarius A*?
Reid, Mark J.
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CitationQuataert, Eliot, Ramesh Narayan, and Mark J. Reid. 1999. “What Is the Accretion Rate in Sagittarius A*?” The Astrophysical Journal 517 (2): L101–4. https://doi.org/10.1086/312035.
AbstractThe radio source Sagittarius A* at the center of our Galaxy is believed to be a 2.6 x 10(6) M. black hole that accretes gas from the winds of nearby stars. We show that limits on the X-ray and infrared emission from the Galactic center provide an upper limit of similar to 8 x 10(-5) M. yr(-1) on the mass accretion rate in Sgr A*. The advection-dominated accretion flow (ADAF) model favors a rate of less than or similar to 10(-5) M. yr(-1). In comparison, the Bondi accretion rate onto Sgr A*, estimated using the observed spatial distribution of mass-losing stars and assuming noninteracting stellar winds, is similar to 3 x 10(-5) M. yr(-1). Thus, there is rough agreement between the Bondi, the ADAF, and the X-ray-inferred accretion rates for Sgr A*. We discuss uncertainties in these estimates, emphasizing the importance of upcoming observations by the Chandra X-ray Observatory for tightening the X-ray-derived limits.
Citable link to this pagehttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41384923
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