Nonradial g-mode oscillations of warm neutron stars

McDermott, P. N.; Horn, H. M. van; Scholl, James F.

doi:10.1086/161006

Cited by 120 publications

(142 citation statements)

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“…(42) and (43), which come from Eqs. (25)- (28) in the limit of µ → 0, are essentially the same as those derived by McDermott et al (1983) for spheroidal oscillation modes.…”

Section: Formulationsupporting

confidence: 80%

“…The purposes of this paper are to calculate the various oscillation modes of relativistic neutron stars with a solid crust in the relativistic Cowling approximation, and to discuss the effects of general relativity on the modal property of the oscillation modes. We regard this paper as an extension of the studies by McDermott et al (1983) and McDermott et al (1988). In Sect.…”

Section: Introductionmentioning

confidence: 92%

“…However, it was the metric perturbations that made it extremely Send offprint requests to: S. Yoshida, e-mail: yoshida@astr.tohoku.ac.jp difficult to treat both analytically and numerically the oscillation modes in relativistic stars. McDermott et al (1983) introduced a relativistic version of the Cowling approximation, in which all the Eulerian metric perturbations δg αβ are neglected in the relativistic oscillation equations derived by Thorne & Campolattaro (1967). Under the relativistic Cowling approximation, they calculated the p-, f -, and g-modes of relativistic f luid neutron star models to examine how the oscillation modes depend on the model properties.…”

Section: Introductionmentioning

confidence: 99%

“…Under the relativistic Cowling approximation, they calculated the p-, f -, and g-modes of relativistic f luid neutron star models to examine how the oscillation modes depend on the model properties. The relativistic Cowling approximation employed by McDermott et al (1983) was shown to be good enough to calculate the p-modes for non-rotating polytropic stars by Lindblom & Splinter (1990), who compared the fully relativistic oscillation frequencies to those obtained in the relativistic Cowling approximation. Assuming slow rotation, Yoshida & Kojima (1997) have also carried out similar computations for the f -and p-modes of polytropic models and they confirmed the good applicability of the relativistic Cowling approximation.…”

Section: Introductionmentioning

confidence: 99%

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Nonradial oscillations of neutron stars with a solid crust

Yoshida¹,

Lee²

2002

A&A

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Abstract. Nonradial oscillations of relativistic neutron stars with a solid crust are computed in the relativistic Cowling approximation, in which all metric perturbations are ignored. For the modal analysis, we employ three-component relativistic neutron star models with a solid crust, a fluid core, and a fluid ocean. As a measure for the relativistic effects on the oscillation modes, we calculate the relative frequency difference defined as δσ/σ ≡ (σ GR − σ N )/σ GR , where σ GR and σ R are, respectively, the relativistic and the Newtonian oscillation frequencies. The relative difference δσ/σ takes various values for different oscillation modes of the neutron star model, and the value of δσ/σ for a given mode depends on the physical properties of the models. We find that |δσ/σ| is less than ∼0.1 for most of the oscillation modes we calculate, although there are a few exceptions such as the fundamental (nodeless) toroidal torsional modes in the crust, the surface gravity modes confined in the surface ocean, and the core gravity modes trapped in the fluid core. We also find that the modal properties, represented by the eigenfunctions, are not strongly affected by introducing general relativity. It is however shown that the mode characters of the two interfacial modes, associated with the core/crust and crust/ocean interfaces, have been interchanged between the two through an avoided crossing when we move from Newtonian dynamics to general relativistic dynamics.

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“…(42) and (43), which come from Eqs. (25)- (28) in the limit of µ → 0, are essentially the same as those derived by McDermott et al (1983) for spheroidal oscillation modes.…”

Section: Formulationsupporting

confidence: 80%

Section: Introductionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Nonradial oscillations of neutron stars with a solid crust

Yoshida¹,

Lee²

2002

A&A

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“…Nonradial oscillations have been studied in detail for NSs both in isolation (McDermott, Van Horn, & Scholl 1983;Finn 1987;McDermott, Van Horn, & Hansen 1988;McDermott 1990;Reisenegger & Goldreich 1992;Strohmayer 1993) and accreting (McDermott & Taam 1987;Bildsten & Cutler 1995, hereafter BC95;Bildsten, Ushomirsky, & Cutler 1996, hereafter BUC96;Strohmayer & Lee 1996;Bildsten & Cumming 1998). To solve the nonradial perturbations on a rotating NS we follow BUC96, but we also include additional new strategies that assist in solving these equations.…”

Section: Nonradial Oscillations In a Thin Shellmentioning

confidence: 99%

Unstable Nonradial Oscillations on Helium‐burning Neutron Stars

Piro

Bildsten

2004

ApJ

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Material accreted onto a neutron star can stably burn in steady state only when the accretion rate is high (typically super-Eddington) or if a large flux from the neutron star crust permeates the outer atmosphere. For such situations we have analyzed the stability of nonradial oscillations, finding one unstable mode for pure helium accretion. This is a shallow surface wave that resides in the helium atmosphere above the heavier ashes of the ocean. It is excited by the increase in the nuclear reaction rate during the oscillations, and it grows on the timescale of a second. For a slowly rotating star, this mode has a frequency !=ð2 Þ % ð20 30 HzÞ½lðl þ 1Þ=2 1=2 , and we calculate the full spectrum that a rapidly rotating (330 Hz) neutron star would support. The short-period X-ray binary 4U 1820À30 is accreting helium-rich material and is the system most likely to show this unstable mode, especially when it is not exhibiting X-ray bursts. Our discovery of an unstable mode in a thermally stable atmosphere shows that nonradial perturbations have a different stability criterion than the spherically symmetric thermal perturbations that generate type I X-ray bursts.

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Non‐radial fluid oscilation modes of color superconducting self‐bound stars

Flores

Lugones

2014

Astron Nachr

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We investigate the effect of color superconductivity on the non-radial oscillations of pure self-bound quark stars using an equation of state in the framework of the MIT bag model. The equations of non-radial oscillations are integrated within the Cowling approximation in order to determine the frequency of the fundamental mode and of the first and second pressure modes. We employ several parametrizations of the equation of state that result in a maximum mass larger than the mass of the recently observed PSR J1614-2230 and PSR J0348-0432 with M ≈ 2 M . The pulsation frequencies are compared with the corresponding modes of quark stars without pairing. For the fundamental mode, the oscillation frequency is typically 2-3 kHz. Parametrizations of the equations of state with larger values of the pairing gap Δ tend to give smaller values of the frequency. For the first and second pressure modes, the frequencies lie in the range 5-10 kHz for stars with masses above 1.5 M and diverge as the mass of the star tends to zero. From the numerical results we obtain parabolic fittings of the frequency of the fundamental mode as a function of the gravitational redshift at the surface of the star. For the p1 and p2 modes we find power law fittings that are rather independent of the parametrization of the equations of state. The here obtained results can be used to extract details about the internal composition of compact stars from observed modes of pulsation.

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Nonradial g-mode oscillations of warm neutron stars

Cited by 120 publications

References 0 publications

Nonradial oscillations of neutron stars with a solid crust

Nonradial oscillations of neutron stars with a solid crust

Unstable Nonradial Oscillations on Helium‐burning Neutron Stars

Non‐radial fluid oscilation modes of color superconducting self‐bound stars

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