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Dissertation/Thesis Abstract

Non-radial fluid pulsation modes of compact stars
by Asbell, Jessica Lee, M.S., California State University, Long Beach, 2016, 70; 10150591
Abstract (Summary)

The observation of gravitational waves from compact stars (neutron and quark stars) is a promising method of determining their internal composition. This research presents the details and results for calculations of some of the principal modes of compact star oscillations, by which they radiate gravitational waves. These are: the f-modes, p-modes, and g-modes. We find that for the same stellar mass, the f-modes for quark stars are higher in frequency than for neutron stars. The p-mode frequency of quark stars decrease with stellar mass, displaying an opposite trend to that of neutron stars. Two-component models were also considered. A core-ocean model was examined for a neutron star, using a polytropic equation of state (EOS), and a core-crust model for a quark star, using a bag model EOS. We find that g-mode oscillations in neutron star oceans depend on the dominant chemical species of the ocean as well as the mass of the underlying core. The addition of a solid crust onto a quark star increases the frequencies, attributable to shear stresses between the core and crust. These results pave the way to model and contrast the gravitational wave signals emitted by oscillating compact stars.

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 56/01M(E), Masters Abstracts International
Subjects: Astrophysics, Physics, Astronomy
Keywords: Gravitational waves, Neutron stars, Quark stars
Publication Number: 10150591
ISBN: 978-1-369-05357-9
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