Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341503m&link_type=abstract
American Astronomical Society, AAS Meeting #213, #415.03; Bulletin of the American Astronomical Society, Vol. 41, p.226
Astronomy and Astrophysics
Astronomy
Scientific paper
Using a set of dynamically evolving Fokker-Planck simulations, we have examined the mass segregation of stars within the Galactic Nucleus. The models initially include a central seed black hole which is fed mass from the surrounding stellar population due to tidal disruptions of stars, stellar collisions, and stellar evolution. All mass loss due to stellar collisions and tidal disruptions is fed to the central black hole due to the proximity of these events to the black hole. A preset fraction of mass loss due to stellar evolution is allowed to be fed to the central black hole and the remainder is assumed to be ejected from the nucleus. This preset fraction is a model parameter that can be varied from 0 to 1. The initial stellar population has initial masses from 0.1 to 100 solar masses. In addition to using the Kroupa mass function models using pure power laws are also examined. As the stellar population evolves possible stellar end states are black holes, neutron stars, and white dwarfs. In the best fitting model of the Galactic Nucleus the region closest to the central black hole is dominated by stellar remnants due to the depletion of normal stars due to stellar collisions. At larger radii the dominate depletion mechanism is tidal disruptions. In this region the most massive stellar mass groups have a power-law density slopes of -7/4. Less massive stellar species have progressively smaller slopes that approach -3/2.
Cohn Haldan N.
Lugger Phyllis Minnie
Murphy Brian William
Phifer Kimberly A.
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