[Previous] | [Session 27] | [Next]
R. M. Salow (Ohio University)
The twin brightness peaks in the nucleus of M31, along with asymmetries in nuclear kinematic profiles obtained from both ground- and space-based data, suggest the presence of an underlying eccentric disk of stars orbiting a supermassive black hole. I have developed a method for constructing approximate self-consistent models of weakly self-gravitating, finite dispersion eccentric stellar disks around central black holes. The disks are fixed in a frame rotating at a constant precession speed, and are built by an iteration scheme in which a disk is populated by quasi-periodic orbits using a distribution function written in terms of the Kepler integrals of motion. I will present results from a grid of models computed to constrain the mass of the central black hole in M31. In particular, a statistically valid black hole mass will be given, and the properties of the disk that best-fits recent nuclear observations will be discussed. The central mass to be reported represents the most well-constrained value to date, since it is obtained using only the most recent high-resolution kinematic and photometric profiles. I have also developed an n-body code which is well suited for stability studies of disk systems with high-eccentricity orbits. Preliminary results on the stability of a particle realization of the best-fit model will be presented.
This research was supported by NSF CAREER grant AST 97-03036
[Previous] | [Session 27] | [Next]
Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.