Physics
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........2q&link_type=abstract
Thesis (PH.D.)--MONTANA STATE UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 57-03, Section: B, page: 18
Physics
Scientific paper
The neutron star thermal calculation is to simulate how temperatures of neutron stars will evolve with time. The ultrahigh density of neutron stars (10^ {15}g cm^{-3}) is a physical condition that cannot be realized in a laboratory so far, and that implies serious theoretical difficulties. Our work on neutron star thermal evolution is to calculate the cooling history of the star and to eliminate some theoretical uncertainties by comparing with the observational data. Among them, the thermal effects of strong magnetic fields, crust breaking, axion emission and neutrino magnetic dipole moment are the four projects we have worked on. The results we obtained are encouraging for all four cases. We found that a magnetic neutron star will maintain a relatively high temperature for a period longer than a non-magnetic star. In the case of crust breaking, our calculations show that for an ideal lattice, the heating due to crust breaking is significant, while for an imperfect lattice, it is not. By including axion emission and effects of neutrino magnetic dipole moment into the neutron star cooling calculations and by comparing with the observational data, we are able to obtain limits on some theoretical parameters, i.e. the mass of axions and neutrino magnetic dipole moment. Also we developed a new way to connect theoretical calculations and observational data through light curves. Theoretical constructions of light curves and comparison with observational data enable us to determine the configurations of magnetic fields and the mechanisms of the emission near the surface of neutron stars.
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