Growth and Evolution of the Central Black Hole in the Galactic Nucleus

Details Growth and Evolution of the Central Black Hole in the Galactic Nucleus Growth and Evolution of the Central Black Hole in the Galactic Nucleus

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341504p&link_type=abstract

American Astronomical Society, AAS Meeting #213, #415.04; Bulletin of the American Astronomical Society, Vol. 41, p.226

Astronomy and Astrophysics

Astronomy

Scientific paper

We have created a set of dynamically evolving models of the Milky Way Galactic Nucleus using the direct Fokker-Planck method. A variety of initial conditions are examined. The mass functions used include the Salpeter and the Kroupa mass functions. The initial mass range extends from 0.1 to 100.0 solar masses. The analytic fitting formulas of Hurley, Pols, and Tout are used to approximate the evolution of stars as a function of mass and metallicity. Initially, all of the models contain a small seed black hole surrounded by an unevolved stellar cluster. The growth of the central black hole is fueled by this stellar population via (1) tidal disruption of stars, (2) physical collisions between stars, and (3) normal stellar evolution. For the Milky Way Galactic Nucleus, stellar evolution and the loss cone are the predominant mass-loss mechanism. The amount of mass allowed to be fed to the central black hole via stellar evolution is varied. The best fitting model closely matches observational data sets of the present-day mass distribution and central black hole mass of 3-4 million solar masses in the Galactic Nucleus.

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