Adiabatic Index of Dense Matter and Damping of Neutron Star Pulsations

Abstract

The adiabatic index Gamma_1 for perturbations of dense matter is studied under various physical conditions which can prevail in neutron star cores. The dependence of Gamma_1 on the composition of matter (in particular, on the presence of hyperons), on the stellar pulsation amplitude, and on the baryon superfluidity is analyzed. Timescales of damping of stellar pulsations are estimated at different compositions, temperatures, and pulsation amplitudes. Damping of pulsations by bulk viscosity in the neutron-star cores can prevent the stars to pulsate with relative amplitudes > (1-15)% (depending on the composition of matter).

5 pages, 2 figures, accepted for publication in A&A

References in corpus (4)

• Neutrino Emission from Neutron Stars
• Effect of hyperon bulk viscosity on neutron-star r-modes
• Bulk viscosity in superfluid neutron star cores. III. Effects of ${\Sigma }^{-}$ hyperons
• Bulk viscosity in superfluid neutron star cores. II. Modified Urca processes in $npe\mu$ matter

Cited by in corpus (37)

• Phase transition effects on the dynamical stability of hybrid neutron stars
• Stable magnetic equilibria and their evolution in the upper main sequence, white dwarfs, and neutron stars
• Extreme Matter meets Extreme Gravity: Ultra-heavy neutron stars with crossovers and first-order phase transitions
• Asteroseismology: radial oscillations of neutron stars with realistic equation of state
• Emergence of microphysical bulk viscosity in binary neutron star post-merger dynamics
• The sum of Love: Exploring the effective tidal deformability of neutron stars
• Bulk viscosity in 2SC quark matter
• Oscillations of hot, young neutron stars: Gravitational wave frequencies and damping times
• Bulk viscosity in relativistic fluids: from thermodynamics to hydrodynamics
• Neutron Stars with Baryon Number Violation, Probing Dark Sectors
• A reliable description of the radial oscillations of compact stars
• Neutron star collapse and gravitational waves with a non-convex equation of state
• Constraining equation of state groups from $g$-mode asteroseismology
• Thermodynamics of uncharged relativistic multifluids
• The baryon coupling scheme in an unified SU(3) and SU(6) symmetry formalism
• Thermal Evolution of a Pulsating Neutron Star
• Starquakes in millisecond pulsars and gravitational waves emission
• Probing elastic quark phases in hybrid stars with radius measurements
• Two first-order phase transitions in hybrid compact stars: higher-order multiplet stars, reaction modes and intermediate conversion speeds
• R-modes and neutron star recycling scenario
• Oscillations of superfluid hyperon stars: decoupling scheme and g-modes
• Hyperon softening of the EOS of dense matter and the spin evolution of isolated neutron stars
• Prior probability distributions of neutron star crust models
• Hyperonic neutron stars: reconciliation between nuclear properties and NICER and LIGO/VIRGO results
• Leptonic contribution to the bulk viscosity of nuclear matter
• Dynamic migration of rotating neutron stars due to a phase transition instability
• Non-equilibrium effects on stability of hybrid stars with first-order phase transitions
• Frozen and $\beta$-equilibrated $f$ and $p$ modes of cold neutron stars: nuclear metamodel predictions
• The impact of nuclear reactions on the neutron-star g-mode spectrum
• Formulating the r-mode problem for slowly rotating neutron stars
• Neutron stars: A novel equation of state with induced surface tension
• Measuring spin in coalescing binaries of neutron stars showing double precursors
• Nonradial oscillations of stratified neutron stars with solid crusts: Mode characterization and tidal resonances in coalescing binaries
• Gravitational waves from post-merger radially-oscillating millisecond pulsars
• Simulating bulk viscosity in neutron stars. I. Formalism
• Inertial modes in stratified rotating neutron stars : An evolutionary description
• Static Charged Polytropic Spheres with a Cosmological Constant: Physical Acceptability and Trapped Orbits