Stability of nonradial oscillations of cold nonrotating neutron stars

Battiston, L.; Cazzola, P.; Lucaroni, L.

doi:10.1007/bf02815343

Cited by 18 publications

(22 citation statements)

References 10 publications

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“…Using the ADM formalism, a first order hyperbolic evolution system is obtained, which is suitable for numerical integration without further manipulations (as was required in the Regge-Wheeler gauge). In this gauge (which is related to a gauge introduced for nonrotating stars in [27]), the symmetry between the polar and axial equations becomes directly apparent.…”

Section: Oscillations and Stabilitymentioning

confidence: 99%

Rotating Stars in Relativity

Stergioulas

2003

Living Rev. Relativ.

436

390

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Rotating relativistic stars have been studied extensively in recent years, both theoretically and observationally, because of the information they might yield about the equation of state of matter at extremely high densities and because they are considered to be promising sources of gravitational waves. The latest theoretical understanding of rotating stars in relativity is reviewed in this updated article. The sections on the equilibrium properties and on the nonaxisymmetric instabilities in f-modes and r-modes have been updated and several new sections have been added on analytic solutions for the exterior spacetime, rotating stars in LMXBs, rotating strange stars, and on rotating stars in numerical relativity.Electronic Supplementary MaterialSupplementary material is available for this article at 10.12942/lrr-2003-3.

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Section: Oscillations and Stabilitymentioning

confidence: 99%

Rotating Stars in Relativity

Stergioulas

2003

Living Rev. Relativ.

436

390

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“…We have presented the derivation of the perturbation equations for slowly rotating relativistic stars using the BCL gauge, which was first used by Battiston et al in 1971. This gauge is defined by setting the metric perturbations α , h , h and h to zero.…”

Section: Discussionmentioning

confidence: 99%

“…For more than 40 yr, it was quite common to work in the Regge–Wheeler gauge (Regge & Wheeler 1957), although some groups have used different gauges or the gauge‐invariant formulation of Moncrief (1974). In a series of papers devoted to the study of the stability properties of non‐radial oscillations in relativistic non‐rotating stars, Battiston, Cazzola & Lucaroni introduced in 1971 a different gauge, which, however, has not received much attention since (Battiston, Cazzola & Lucaroni 1971; Cazzola & Lucaroni 1972, 1974, 1978; Cazzola, Lucaroni & Semenzato 1978a,b).…”

Section: Introductionmentioning

confidence: 99%

“…We note again that this gauge was actually introduced thirty years ago by Battiston et al (1971) to derive the perturbation equations for non‐radial oscillations of non‐rotating neutron stars and to investigate their stability properties in a subsequent series of papers (Cazzola & Lucaroni 1972, 1974, 1978; Cazzola, Lucaroni & Semenzato 1978a,b). The first paper is of particular relevance, as they show that this gauge does not contain any further gauge freedom and establish the relation with the Regge–Wheeler gauge.…”

Section: Introductionmentioning

confidence: 99%

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Evolution equations for the perturbations of slowly rotating relativistic stars

Ruoff

Stavridis

Kokkotas

2002

Monthly Notices of the Royal Astronomical Society

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We present a new derivation of the equations governing the oscillations of slowly rotating relativistic stars. Previous investigations have been mostly carried out in the Regge–Wheeler gauge. However, in this gauge the process of linearizing the Einstein field equations leads to perturbation equations in a form that cannot be used to perform numerical time evolutions. It is only through the tedious process of combining and rearranging the perturbation variables in a clever way that the system can be cast into a set of hyperbolic first‐order equations, which is then well suited for the numerical integration. The equations remain quite lengthy, and we therefore rederive them in a different gauge. Using the ADM formalism, one immediately obtains a first‐order hyperbolic evolution system, which is remarkably simple and can be integrated numerically without many further manipulations. Moreover, the symmetry between the polar and axial equations becomes directly apparent.

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“…The complete set of equations for the perturbations has been derived using the so-called BCL gauge [21] by Ruoff, Stavridis & Kokkotas [22]. The Cowling limit of these equations, which neglects the contribution of the gravitational perturbations, was studied in [23] for polytropic relativistic equations of state.…”

Section: Formulation Of the Problemmentioning

confidence: 99%

Gravitational waves from rotating proto-neutron stars

Ferrari

Gualtieri

Pons

et al. 2004

Class. Quantum Grav.

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Abstract. We study the effects of rotation on the quasi normal modes (QNMs) of a newly born proto neutron star (PNS) at different evolutionary stages, until it becomes a cold neutron star (NS). We use the Cowling approximation, neglecting spacetime perturbations, and consider different models of evolving PNS. The frequencies of the modes of a PNS are considerably lower than those of a cold NS, and are further lowered by rotation; consequently, if QNMs were excited in a sufficiently energetic process, they would radiate waves that could be more easily detectable by resonant-mass and interferometric detectors than those emitted by a cold NS. We find that for high rotation rates, some of the g-modes become unstable via the CFS instability; however, this instability is likely to be suppressed by competing mechanisms before emitting a significant amount of gravitational waves.

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Stability of nonradial oscillations of cold nonrotating neutron stars

Cited by 18 publications

References 10 publications

Rotating Stars in Relativity

Rotating Stars in Relativity

Evolution equations for the perturbations of slowly rotating relativistic stars

Gravitational waves from rotating proto-neutron stars

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