Currently, we lack a means of identifying the type of matter at the core of compact stars, but in the future, we may be able to use gravitational wave signals produced by fluid oscillations inside compact stars to discover new phases of dense matter. To this end, we study the fluid perturbations inside compact stars such as Neutron Stars (NS) and Strange Quark Stars (SQS), focusing on modes that couple to gravitational waves (GWs). Using a modern equation of state for quark matter that incorporates interactions at moderately high densities, we implement an efficient computational scheme to solve the oscillation equations in the framework of General Relativity, and determine the complex eigenfrequencies that describe the oscillation and damping of the non-radial fluid modes. We find that the f- mode frequency only weakly distinguishes NS from SQS. However, we do find that the p- mode has a strong discriminating signature between the two models. In addition we study the impact of parameters of the SQS equation of state on the oscillation spectra. Finally, we discuss the significance of our results for future detection of these modes through gravitational waves.
|Commitee:||Ojeda-Aristizabal, Claudia, Papp, Zoltan|
|School:||California State University, Long Beach|
|Department:||Physics and Astronomy|
|School Location:||United States -- California|
|Source:||MAI 57/01M(E), Masters Abstracts International|
|Subjects:||Astrophysics, Physics, Astronomy|
|Keywords:||Gravitational waves, Neutron stars, Quark stars|
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