The radial oscillations of neutron stars

Glass, E. N.; Lindblom, Lee

doi:10.1086/190885

Cited by 52 publications

(48 citation statements)

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“…However, these are not all the modes the stars possess. It is well known that NSs in GR are characterized by a set of radial normal modes, i.e., not damped modes, that become unstable modes beyond the maximum mass NS for a given equation of state (EOS) [26][27][28][29][30][31][32]. Clearly in GR, radial perturbations cannot propagate gravitational radiation outside of the NS, and thus these modes play no role during the ringdown phase.…”

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confidence: 99%

Axial quasinormal modes of neutron stars in R2 gravity

et al. 2018

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The spectrum of frequencies and characteristic times that compose the ringdown phase of gravitational waves emitted by neutron stars carry information about the matter content (the equation of state) and the underlying theory of gravity. Typically, modified theories of gravity introduce additional degrees of freedom/fields, such as scalars, which result in new families of modes composing the ringdown spectrum. One simple but physically promising candidate is R 2 gravity, which effectively introduces an additional massive scalar field that couples non-minimally to gravity, resulting in scalarized neutron stars. Here we show that the ringdown spectrum of R 2 neutron stars is much richer and fundamentally different from the spectrum in GR, possessing for instance ultra long lived modes that can propagate away from the star in the form of scalar gravitational radiation.

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confidence: 99%

Axial quasinormal modes of neutron stars in R2 gravity

et al. 2018

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“…whereτ d = (τ d1 + τ d2 )/40s, the gravitational radiation can damp the radial oscillations very efficiently. The frequency of the gravitational waves is euqal to ω = 2π/τ , where τ is close to 5×10 −4 s for a typical neutron-star model (Glass & Lindblom 1983) (corrected for the gravitational redshift) with mass M ∼ 1.8M ⊙ and radius R ∼ 10 6 cm. The strength of the waves can be estimated using the quadrupole approximation to the Einstein field equations (Thorne 1987).…”

Section: Damping Of Radial Oscillationsmentioning

confidence: 79%

Gravitational Waves from Phase Transitions of Accreting Neutron Stars

Cheng

Dai

1998

ApJ

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We propose that when neutron stars in low-mass X-ray binaries accrete sufficient mass and become millisecond pulsars, the interiors of these stars may undergo phase transitions, which excite stellar radial oscillations. We show that the radial oscillations will be mainly damped by gravitational-wave radiation instead of internal viscosity. The gravitational waves can be detected by the advanced Laser Interferometer Gravitational-Wave Observatory at a rate of about three events per year.

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“…The first exhaustive compilation of radial modes for various zero temperature EOSs was presented by Glass & Lindblom in 1983 [2]. Later studies by Väth & Chanmugan [3] complemented and corrected earlier studies and also considered the case of strange quark stars.…”

Section: Introductionmentioning

confidence: 99%

Radial Oscillations of Color Superconducting Quark Stars

Flores¹

2011

Proceedings of 4th School on Cosmic Rays and Astrophysics — PoS(CRA School)

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We investigate the effect of the color-flavor locking pairing pattern on the adiabatic radial oscillations of pure self-bound quark stars using an equation of state in the framework of the MIT Bag model. We integrate the equations of relativistic radial oscillations to determine the fundamental and the first excited oscillation modes for several parameterizations of the equation of state. For low mass stars we find that the period of the fundamental mode is typically ∼ 0.1 ms and has a small dependence on the parameters of the equation of state. For large mass stars the effect of color-flavor locking is related to the rise of the maximum mass with increasing ∆. As for unpaired quark stars, the period of the fundamental mode becomes divergent at the maximum mass but now the divergence is shifted to large masses for large values of the pairing gap ∆. As a consequence, the oscillation period is strongly affected by color superconductivity for stars with M 1.5 M . We further discuss the excitation and damping of the modes and their potential detectability during violent transient phenomena.4th School on Cosmic Rays and Astrophysics

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The radial oscillations of neutron stars

Cited by 52 publications

References 0 publications

Axial quasinormal modes of neutron stars in R2 gravity

Axial quasinormal modes of neutron stars in R2 gravity

Gravitational Waves from Phase Transitions of Accreting Neutron Stars

Radial Oscillations of Color Superconducting Quark Stars

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