Mathematics – Logic
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt........27p&link_type=abstract
Thesis (PH.D.)--HARVARD UNIVERSITY, 1982.Source: Dissertation Abstracts International, Volume: 43-09, Section: B, page: 2935.
Mathematics
Logic
3
Scientific paper
Chapter one investigates the late stages of core collapse in a star cluster using a simplified two-region model. The results indicate that self-interactions with core stars are the dominant evolutionary mechanism, leading to the evaporation of stars from the core. These stars do not escape from the entire cluster because the collapse causes the core radius to shrink below their orbital pericenters. The homological evaporation model gives a good description of the time dependent behavior of the system. However, the rate of collapse may be different from that of the early stages. Chapter two presents a method of preserving galaxy -sized (10('12) M(,(CIRCLE))) perturbations in a population of massive neutrinos. Neutrinos with a rest mass on the order of 100 keV will preserve and amplify such perturbations but must decay before today so as not to violate limits on the present mass density of the universe. A population of neutrinos with a rest mass on the order of 100 eV may be able to become non-relativistic and pick up the perturbations before the heavier neutrinos decay. Chapter three examines the question of whether spherically symmetric secondary infall can produce massive galactic halos with a density profile proportional to r(' -2). An extensive series of numerical experiments shows that the initial conditions that would produce a shallow profile also lead to collective relaxation that steepens the actual final profile. As a result, profiles as shallow as r('-2) are never formed. Chapter four uses a radial variation of the HI content of the spiral galaxies in Coma cluster, most likely due to ram pressure stripping, to decide which galaxies have been near the center of the cluster and which have not. When combined with a dynamical model this information constrains the ratio of the radial to the tangential components of the velocity dispersion. A radial variation in the relation between the central surface brightness and total luminosity of ellipticals can be similarly used. The results from the two sets of data show that the velocity dispersion cannot be very radially biased inside 7 core radii.
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