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Gravitational Wave asteroseismology revisited
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The frequencies and damping times of the non radial oscillations of neutron stars are computed for a set of recently proposed equations of state (EOS) which describe matter at supranuclear densites. These EOS are obtained within two different approaches, the nonrelativistic nuclear many-body theory and the relativistic mean field theory, that model hadronic interactions in different ways leading to different composition and dynamics. Being the non radial oscillations associated to the emission of gravitational waves, we fit the eigenfrequencies of the fundamental mode and of the first pressure and gravitational-wave mode (polar and axial) with appropriate functions of the mass and radius of the star, comparing the fits, when available, with those obtained by Andersson and Kokkotas in 1998. We show that the identification in the spectrum of a detected gravitational signal of a sharp pulse corresponding to the excitation of the fundamental mode or of the first p-mode, combined with the knowledge of the mass of the star - the only observable on which we may have reliable information - would allow to gain interesting information on the composition of the inner core. We further discuss the detectability of these signals by gravitational detectors.
Forward citations
Cited by 8 Pith papers
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Reaction-constrained composition \(g\)-modes in neutron stars with antikaon condensates, hyperons, and \(\Delta(1232)\) resonances
Antikaon condensates create a distinct composition g-mode that survives fast kaon equilibration, while strong Delta equilibration suppresses the Delta-driven mode except where a frozen Lambda gradient survives.
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Out-of-Equilibrium Effects in Non-Radial Relativistic Stellar Perturbations: A Model-Agnostic Formulation and Mode Analysis
A general framework for incorporating arbitrary nonequilibrium corrections into linear non-radial relativistic stellar perturbations without specifying constitutive relations.
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Radial Oscillations of Viscous Stars
Viscosity damps neutron-star radial modes on ms timescales, shifts frequencies by up to ~1% at ζ∼10^30 g/cm/s, produces overdamped modes above ∼10^31, and cannot stabilize unstable stars in Eckart or BDNK theory.
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Examining the influence of anisotropy on the fundamental mode of nonradial oscillation in neutron stars on a complete general relativistic scheme
Pressure anisotropy in strange quark stars measurably changes the f-mode oscillation frequency and the dimensionless tidal deformability, with positive anisotropy increasing mass and deformability while lowering the f...
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Magnetic effects on fundamental modes in rotating neutron stars with a purely toroidal magnetic field
Even with both rotation and a toroidal magnetic field, neutron star fundamental-mode frequencies stay quasi-linear in compactness and T/|W|, with magnetization-dependent slopes, and the f_2f/f_F ratio can help constra...
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Role of density profile of sub-GeV dark matter in the properties of dark matter admixed quark stars with Bayesian analysis of dark-NJL model
A model of quark stars with a variable dark matter density profile claims sub-GeV dark matter can satisfy all current compact star constraints.
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Effect of Dark matter and $\sigma$-cut potential on radial and non-radial oscillation modes in neutron stars
Dark matter-admixed neutron stars oscillate at higher f- and p1-mode frequencies than ordinary or σ-cut models, while quasi-universal oscillation relations still hold.
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Phase transitions in neutron stars and their links to gravitational waves
Review of neutron star dense matter, hadron-quark phase transitions, and potential g-mode signatures in gravitational waves from multimessenger observations.
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