Hydrodynamical Accretion Onto Sgr A* From Distributed Point Sources

Details Hydrodynamical Accretion Onto Sgr A* From Distributed Point Sources Hydrodynamical Accretion Onto Sgr A* From Distributed Point Sources

1997-08-10

arxiv.org/abs/astro-ph/9708089v1

ApJ, 1997, vol. 488, p. L149

Astronomy and Astrophysics

Astrophysics

17 pages, including 4 PS figures; uses aasms4.sty; accepted by ApJL

Scientific paper

10.1086/310925

Spectral and kinematic studies suggest that the nonthermal radio source Sgr A*, located at the center of the Milky Way, is a supermassive compact object with a mass 2-3 million solar masses. Winds from nearby stars, located approximately 0.06 pc to the east of Sgr A*, should, in the absence of any outflow from the putative black hole itself, be accreting onto this object. We report the results of the first 3D Bondi-Hoyle hydrodynamical numerical simulations of this process under the assumption that the Galactic center wind is generated by several different point sources (here assumed to be 10 pseudo-randomly placed stars). Our results show that the accretion rate onto the central object can be higher than in the case of a uniform flow since wind-wind shocks dissipate some of the bulk kinetic energy and lead to a higher capture rate for the gas. However, even for this highly non-uniform medium, most of the accreting gas carries with it a relatively low level of specific angular momentum, though large transient fluctuations can occur. Additionally, the post-bow-shock focusing of the gas can be substantially different than that for a uniform flow, but it depends strongly on the stellar spatial distribution. We discuss how this affects the morphology of the gas in the inner 0.15 pc of the Galaxy and the consequences for accretion disk models of Sgr A*.

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