Temperature Effects on Core g-modes of Neutron Stars

Abstract

Neutron stars provide a unique physical laboratory to study the properties of matter at high density. We study a diagnostic of the composition of high-density matter, namely, g-mode oscillations, which are driven by buoyancy forces. These oscillations can be excited by tidal forces and couple to gravitational waves. We extend prior results for the g-mode spectrum of cold neutron star matter to temperatures that are expected to be achieved in neutron star mergers using a parameterization for finite-temperature effects recently proposed by Raithel, Özel and Psaltis. We find that the g-modes of canonical mass neutron stars ($\approx$1.4$M_{\odot }$) are suppressed at high temperature, and core $g$-modes are supported only in the most massive ($\ge$2$M_{\odot }$) of hot neutron stars.

8 pages, 4 figures

References in corpus (7)

• Universal Relations for Neutron Star F-Mode and G-Mode Oscillations
• Finite-temperature extension for cold neutron star equations of state
• Effect of hyperons on f-mode oscillations in Neutron Stars
• Effects of short-range correlation reduced kinetic symmetry energy in heavy-ion collisions at intermediate energies
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Cited by in corpus (10)

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• Neutron-star seismology with realistic, finite-temperature nuclear matter
• Suppression of composition $g$-modes in chemically-equilibrating warm neutron stars
• Constraining the $f$-mode oscillations frequency in Neutron Stars through Universal Relations in the realm of Energy-Momentum Squared Gravity
• $f$ and $p$ mode oscillation of proto-neutron stars with systematic variation of the nucleon effective mass
• Modification of the universal relation between mass, radius and nonradial $f$-mode oscillation in proto-neutron stars
• Investigating Universal Relations in Compact Stars featuring $\Delta -$Admixed Exotic Dense Matter