Self-Consistent Models of Eccentric Nuclear Disks

Details Self-Consistent Models of Eccentric Nuclear Disks Self-Consistent Models of Eccentric Nuclear Disks

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dda....31.1002s&link_type=abstract

American Astronomical Society, DDA Meeting #31, #10.02; Bulletin of the American Astronomical Society, Vol. 32, p.865

Astronomy and Astrophysics

Astronomy

Scientific paper

We have constructed approximate self-consistent models of eccentric stellar disks. Our models include a self-gravitating disk with finite velocity dispersion which precesses about a central black hole. These models are constructed via a self-consistent iteration scheme in which a disk is populated by a sequence of finite-dispersion orbits whose parents are numerically integrated closed periodic orbits. Once an initial model is assumed, a set of uniformly precessing closed periodic orbits is found in the potential of the disk/black hole system, which is then used to construct a new disk using an approximate phase space distribution function written in terms of the integrals of motion in the two-dimensional Kepler problem. This cycle continues until an equilibrium configuration is found. Results show that there exist various combinations of disk precession speed, disk mass, and orbital dispersion for which converged equilibrium disks can be found. Analysis of these models shows that they have rotation and dispersion profiles that resemble those of M31, as observed by the HST Faint Object Camera. We will discuss these similarities, paying particular attention to the asymmetries and fine structure in the profiles. Also, we will consider how the velocity profiles change with changing parameter values, and how the information contained in them can possibly be used to constrain the disk dynamics, disk mass, and black hole mass for systems such as M31 and NGC4486B.

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