Simulating Galaxy Formation

Details Simulating Galaxy Formation Simulating Galaxy Formation

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.586b&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

We describe the first application of a new hydrodynamics method to the problem of galaxy formation. This technique, Adaptive Mesh Refinement (AMR), combines the well-tested methods of Eulerian hydrodynamics with an adaptive method for adding resolution in the form of multiple levels of finer meshes. As a first step we model dark matter and gas with an equilibrium cooling rate. We examine the results from a handful of galactic-sized halos with a spatial dynamic range of about 10^5. The halos form at z ~3, but the disks tend to grow from the inside out with higher angular momentum gas accreting later. The specific angular momentum of the gas disks is comparable to that of their dark matter halos and may be consistent with observed spirals. We discuss the effect of ram pressure stripping.

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