Hydrodynamic Simulations of Galaxy Formation. I. Dissipation and the Maximum Mass of Galaxies
Abstract
We describe an accurate, onedimensional, spherically symmetric Lagrangian hydrodynamics/gravity code, designed to study the effects of radiative cooling and photoionization on the formation of protogalaxies. The code can treat an arbitrary number of fluid shells (representing baryons) and collisionless shells (representing cold dark matter). As a test of the code, we reproduce analytic solutions for the pulsation behavior of a polytrope and for the selfsimilar collapse of a spherically symmetric, cosmological perturbation. In this paper we concentrate on the effects of radiative cooling, examining the ability of collapsing perturbations to cool within the age of the universe. In contrast to, some studies based on orderofmagnitude estimates, we find that cooling arguments alone cannot explain the sharp upper cutoff observed in the galaxy luminosity function.
 Publication:

The Astrophysical Journal
 Pub Date:
 April 1995
 DOI:
 10.1086/175455
 arXiv:
 arXiv:astroph/9410009
 Bibcode:
 1995ApJ...442..480T
 Keywords:

 Astronomical Models;
 Energy Dissipation;
 Galactic Evolution;
 Galactic Mass;
 Gravitation;
 Hydrodynamics;
 Computerized Simulation;
 Finite Difference Theory;
 Luminosity;
 Mathematical Models;
 Photoionization;
 Polytopes;
 Radiative Heat Transfer;
 Astrophysics;
 GALAXIES: FORMATION;
 HYDRODYNAMICS;
 METHODS: NUMERICAL;
 Astrophysics
 EPrint:
 33 pages, uuencoded compressed postscript with figures, Ap.J. (in press), corrections to axes in Fig 1