Dissertation/Thesis Abstract

Calculations of the spectrum of non-radial oscillations in neutron stars
by Bandari, Anashe, M.S., California State University, Long Beach, 2014, 44; 1526891
Abstract (Summary)

Neutron stars are among the densest objects in the universe and are one possible end result of stellar evolution. They contain forms (phases) of matter that are not possible to create under terrestrial conditions. Therefore, we can learn about new phases of matter by studying aspects of neutron stars. In particular, the way the fluid comprising the neutron star oscillates as a result of perturbations to the pressure and density of the star can lead to a variety of interesting phenomena, including the emission of gravitational waves. These can be modeled using theory and tested by observations. In this thesis, we focus on the p-mode oscillations, which are a type of spheroidal oscillation driven by internal pressure fluctuations. These are acoustic modes with very short time periods. We have calculated, using both analytical and numerical methods, the p-mode periods in a simple model of dense relativistic stars, of which neutron stars are standard examples. In a local analysis, we found a 0.3 ms upper limit on oscillation periods analytically. We then used a numerical analysis to find exact solutions for these periods, which agreed with our upper limit calculation. Our numerical analysis demonstrated that a small spherical harmonic degree has a small effect on the oscillation spectrum, and that a larger spherical harmonic degree introduces a period doubling phenomenon.

Indexing (document details)
Advisor: Jaikumar, Prashanth
Commitee: Gredig, Thomas, Peterson, Michael
School: California State University, Long Beach
Department: Physics and Astronomy
School Location: United States -- California
Source: MAI 53/06M(E), Masters Abstracts International
Subjects: Astrophysics
Keywords: Neutron star oscillation, Nonradial oscillation, Oscillation spectrum, P-mode
Publication Number: 1526891
ISBN: 978-1-321-27691-6
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