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Non-Radial Oscillation Modes of Superfluid Neutron Stars Modeled with CompOSE

Department of Physics and Astronomy, California State University Long Beach, 1250 Bellflower Blvd., Long Beach, CA 90840, USA
Author to whom correspondence should be addressed.
Universe 2018, 4(3), 53;
Received: 16 January 2018 / Revised: 15 February 2018 / Accepted: 24 February 2018 / Published: 9 March 2018
(This article belongs to the Special Issue Compact Stars in the QCD Phase Diagram)
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We compute the principal non-radial oscillation mode frequencies of Neutron Stars described with a Skyrme-like Equation of State (EoS), taking into account the possibility of neutron and proton superfluidity. Using the CompOSE database and interpolation routines to obtain the needed thermodynamic quantities, we solve the fluid oscillation equations numerically in the background of a fully relativistic star, and identify imprints of the superfluid state. Though these modes cannot be observed with current technology, increased sensitivity of future Gravitational-Wave Observatories could allow us to observe these oscillations and potentially constrain or refine models of dense matter relevant to the interior of neutron stars. View Full-Text
Keywords: neutron stars; gravitational waves; equation of state neutron stars; gravitational waves; equation of state

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Jaikumar, P.; Klähn, T.; Monroy, R. Non-Radial Oscillation Modes of Superfluid Neutron Stars Modeled with CompOSE. Universe 2018, 4, 53.

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