Nearly Self-Consistent Disk-Bulge-Halo Models for Galaxies

Details Nearly Self-Consistent Disk-Bulge-Halo Models for Galaxies Nearly Self-Consistent Disk-Bulge-Halo Models for Galaxies

1995-02-09

arxiv.org/abs/astro-ph/9502051v2

Astronomy and Astrophysics

Astrophysics

Resubmission. latex source file (8p, using mn.sty) and uuencoded postscript file with 9 figures.

Scientific paper

We describe methods for setting up self-consistent disk-bulge-halo galaxy models. The bulge and halo distribution functions (\df) are functions of $E$ and $L_z$ only. The halo's flattening and rotation can be specified. The disk \df\ is a function of $E$ and $L_z$ and a third ``integral'', $E_z$, the vertical energy, which is approximately conserved in a warm disk with vertical extent. The models also have finite extent making them suitable for N-body simulation. A simulation of a sample model shows that in practice the models are very close to equilibrium making them ideal for experiments on instabilities in galactic disks. We also present a sequence of models closely resembling the Milky Way mass distribution with 5 exponential scale radii and varying halo mass and radial extent.

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