Computer Science
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........4m&link_type=abstract
Ph.D. Thesis Princeton Univ., NJ.
Computer Science
4
Collapse, Stellar Evolution, Stellar Models, Stellar Systems, Angular Momentum, Density (Mass/Volume), Distribution Functions, Spherical Harmonics, Stellar Temperature
Scientific paper
A numerical technique is applied to the dissipationless collapse of point masses. The numerical scheme involves an expansion of the potential in a radial grid, using spherical harmonics to express the angular dependence. Advantages are an ability to model extremely high density cores in systems, a strong damping of two body interactions, and an efficient algorithm for integrating the equations of motion. A very wide range of initial conditions is considered, with particular emphasis on the initial temperature and clumpiness of the systems. Some simulations consider extremely anisotropic initial conditions and the effects of large angular momenta. The final states of the system are strongly dependent on the initial temperature, but information on the initial inhomogeneity appears to be lost. Large density contrasts are obtainable in systems starting with low temperatures. These systems also appear to give reasonable fits to Hubble or de Vaucouleurs profiles over virtually their entire mass. The distribution function of the final states is computed as a function of energy, and alternatively as a function of energy and angular momentum.
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