Mathematics – Logic
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........39k&link_type=abstract
PhD Dissertation, California Univ. Riverside, CA United States
Mathematics
Logic
Stellar Models, Neutron Stars, Stellar Evolution, Supernovae, Pulsars, Stellar Rotation
Scientific paper
By comparing the rate of supernova explosions in our galaxy to the number of pulsars that are visible we easily notice the disparity between these two numbers. The lack of long period pulsars has also kept the astronomical community wondering for the last two decades. The model presented in this work tries to address this problem which the standard model of neutron stars given by Gold (1968) could not give a complete and adequate account for. At first a two component model of a neutron star is considered. In this model the neutron star is assumed to be made up of two differently charged, differentially rotating and spherically symmetric objects. The magnetic and viscous interactions between the two bodies seem to lead to all the observed properties of a pulsar and more. It is shown that a neutron star passes through three different modes in its lifetime. These modes are the chaotic mode, the pulsar mode and the dead mode. It is also shown that the two component model can easily be extended to include an additional superfluid component which comes in between the two solid parts. Next a phenomenological picture of the evolution of the neutron star as it transits from one mode to the other is described in relation to its loss of mechanical energy. The loss in mechanical energy is modelled to proportionally increase the magnetic damping constant. It is expected that the transition of the neutron star from the chaotic mode to the dead mode is made in a time which could be several orders of magnitude less than what the standard model predicts for the average age of a neutron star (approximately 107 years). Finally the effect of neutrino cooling on the evolution of the neutron star is considered. It is shown that the age of a neutron star is highly dependent upon the initial values of the transverse and longitudinal viscosity of the superfluid matter with which the two solid components are weakly coupled.
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