Physics
Scientific paper
Jan 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996phdt.........5s&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF MAINE, 1996.Source: Dissertation Abstracts International, Volume: 57-04, Section: B, page: 2621.
Physics
3
Scientific paper
A computer program was developed for the simulation of stellar evolution processes in disk galaxies. The computer program is based on a standard n-body approach to galaxy simulation, which utilizes collisionless star particles and a static halo. Hydrodynamic and cloud-particle components were added to the n-body code. All four components (stars, clouds, gas, and halo) exchange mass, energy, and momentum via various evolution processes and gravity. This thesis discusses the physical and numerical issues relevant to the development of the program, and the results of a series of runs. Once initial program development was completed, a number of topics were studied using the program. First, effects of numerical artifacts present in the hydrodynamics were noted and minimized. Response curves for each stellar evolution process were determined. From these, an input parameter set that results in a "near-steady-state" system was estimated. Near-steady-state runs were conducted at low and medium grid resolutions, both showing continued spiral structure and steady mass exchange rates between the four components for at least 10 rotation periods. The input parameter space surrounding the near-steady-state input set was explored in a series of runs, demonstrating the robustness of the steady-state. Increasing the number of star particles from 30,000 to 90,000 showed that relaxation effects, due to the "small" number of particles, are present and not easily reduced when the stellar evolution model is active. The present stellar evolution model can enhance or dampen the spiral density waves, depending on the mass distribution used. The limited scale (number of particles and grid resolution) of these introductory runs made it difficult to determine if bright OB associations formed predominantly in the spiral arms. Particular attention is given to the connection between physical quantities and numerical parameters. Code verification is discussed. A final "Users Manual" chapter is included for those who wish to use and continue developing this program.
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