Nearly Self-Consistent Disc / Bulge / Halo Models for Galaxies

Details Nearly Self-Consistent Disc / Bulge / Halo Models for Galaxies Nearly Self-Consistent Disc / Bulge / Halo Models for Galaxies

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277.1341k&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Vol. 277, NO. 4/DEC15, P.1341, 1995

Astronomy and Astrophysics

Astronomy

130

Scientific paper

We describe methods for setting up self-consistent disc-bulge-halo galaxy models. The bulge and halo distribution functions (DFs) are functions of E and L_z_ only. The halo's flattening and rotation can be specified. The disc 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 disc 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 discs. 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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