Neutron star matter equation of state and gravitational wave emission

Abstract

The EOS of strongly interacting matter at densities ten to fifteen orders of magnitude larger than the typical density of terrestrial macroscopic objects determines a number of neutron star properties, including the pattern of gravitational waves emitted following the excitation of nonradial oscillation modes. This paper reviews some of the approaches employed to model neutron star matter, as well as the prospects for obtaining new insights from the experimental study of gravitational waves emitted by neutron stars.

15 pages, 8 figures. To be published as a Brief Review in Modern Physics Letters A

References in corpus (3)

• Quantum Monte Carlo Calculations of Light Nuclei
• Gravitationally redshifted absorption lines in the X-ray burst spectra of a neutron star
• Stability of the mixed phase in hybrid stars

Cited by in corpus (7)

• Phenomenological Relations for Axial Quasi-normal Modes of Neutron Stars with Realistic Equations of State
• Exotic matter influence on the polar quasi-normal modes of neutron stars with equations of state satisfying the $2M_{\odot }$ constraint
• Imprints of the nuclear symmetry energy on gravitational waves from the axial w-modes of neutron stars
• Breaking the EOS-Gravity Degeneracy with Masses and Pulsating Frequencies of Neutron Stars
• Energy release from hadron-quark phase transition in neutron stars and the axial $w$-mode of gravitational waves
• Probing dense matter in neutron stars with axial w-modes
• Influence of hyperon-hyperon interaction on the properties of neutron stars