Neutron stars and Black Holes are prominent sources of gravitational waves. In any theoretical model of a neutron star that can be applied to calculate the gravitational wave frequencies, we first need to know the radius of the star precisely since the allowed fluid oscillation modes of the star arise from strict boundary conditions at the surface of the star. In this thesis, we present an alternate approach to solving the structure of the neu- tron star and thereby finding the radius. Whereas traditional approaches use r, the dis- tance from the star’s center, as the independent variable and search for the radius by find- ing the zero of the pressure function, we use the dimensionless enthalpy h as the indepen- dent variable and determine the radius simply by stepping to the h = 0 point. We test our method on three different cases. Two of these are simple parameterizations : a polytropic model that approximates neutron star matter and a thermodynamic Bag model that ap- proximates quark star matter. The third is a microscopic, but still simple, model based on nucleon-nucleon interactions that gives a slightly more realistic description of the matter inside neutron stars. In each case, we find that our method gives results that are almost identical to the traditional method, but in a more computationally efficient way. This im- provement should make more involved computations of the gravitational wave spectrum emitted by the star significantly faster.
|Commitee:||Klaehn, Thomas, Gredig, Thomas|
|School:||California State University, Long Beach|
|Department:||Physics and Astronomy|
|School Location:||United States -- California|
|Source:||MAI 81/4(E), Masters Abstracts International|
|Subjects:||Astrophysics, Computational physics|
|Keywords:||astrophysics, computational physics, enthalpy|
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