Stillen beeinträchtigt/Stillen erfolgreich

Kastaun, Cornelia; Nümann-Dulke, Anke; Nispel, Sabine; Becker, Michaela

doi:10.1007/3-540-29434-1_54

Cited by 2 publications

(4 citation statements)

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“…where G µν is the Einstein-tensor, describing the geometry of space-time, and T µν is the energy-momentum-tensor that defines the functional form of energy momentum and stress of the fluid. Since it is very complicated, but not impossible [35,45], to solve this system as such, we will introduce some approximations in studying the problem. First of all, we linearize equations (1) and (2), which means that we constrain our study to small perturbations around the equilibrium.…”

Section: The Perturbation Equationsmentioning

confidence: 99%

“…This is a quite good approximation, both qualitatively and quantitatively, for the higher order p-modes, for the g-modes and the inertial modes while it is only qualitatively good for the f-modes, see for example [28]. Although, most of our understanding on the oscillations of relativistic stars is due to perturbative studies, recently, it has become possible to study stellar oscillations using evolutions of the non-linear equations of motion for the fluid [29,30,31,32,33,34,35,36,37]. Finally, differential rotation is another key issue that is believed to play an important role in the dynamics of nascent neutron stars.…”

Section: Introductionmentioning

confidence: 99%

“…to freeze the spacetime perturbations or in the best case to freeze the radiative part of these perturbations. This was the approach used up to now for most of the studies of the oscillations of fast rotating relativistic stars either in perturbative approaches [43,44] or in non-linear (but axisymmetric) approaches [35,45].…”

Section: Introductionmentioning

confidence: 99%

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Oscillations of rapidly rotating relativistic stars

2008

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Nonaxisymmetric oscillations of rapidly rotating relativistic stars are studied using the Cowling approximation. The oscillation spectra have been estimated by Fourier transforming the evolution equations describing the perturbations. This is the first study of its kind and provides information on the effect of fast rotation on the oscillation spectra while it offers the possibility of studying the complete problem by including space-time perturbations. Our study includes both axisymmetric and nonaxisymmetric perturbations and provides limits for the onset of the secular bar mode rotational instability. We also present approximate formulas for the dependence of the oscillation spectrum from rotation. The results suggest that it is possible to extract the relativistic star's parameters from the observed gravitational wave spectrum

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Section: The Perturbation Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Oscillations of rapidly rotating relativistic stars

2008

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“…Currently, waveform models used to interpret BNS observations do not include the merger and post-merger regimes. Although numerical-relativity (NR) simulations of BNS mergers have made tremendous progress in recent years [42][43][44][45][46][47][48][49][50][51][52], we do not yet have complete models of the inspiral, merger, and post-merger regime, as we do for BBH systems [53][54][55][56]. The waveform models used for current GW analyses are either truncated prior to merger (this is the case for all models used to analyse GW170817 [12]), or are BBH models through the merger and ringdown (which are included in this study).…”

Section: Introductionmentioning

confidence: 99%

Relevance of tidal effects and post-merger dynamics for binary neutron star parameter estimation

Dudi¹,

Pannarale

Dietrich

et al. 2018

Phys. Rev. D

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Measurements of the properties of binary neutron star systems from gravitational-wave observations require accurate theoretical models for such signals. However, current models are incomplete, as they do not take into account all of the physics of these systems: some neglect possible tidal effects, others neglect spin-induced orbital precession, and no existing model includes the postmerger regime consistently. In this work, we explore the importance of two physical ingredients: tidal interactions during the inspiral and the imprint of the post-merger stage. We use complete inspiral-merger-post-merger waveforms constructed from a tidal effective-one-body approach and numerical-relativity simulations as signals against which we perform parameter estimates with waveform models of standard LIGO-Virgo analyses. We show that neglecting tidal effects does not lead to appreciable measurement biases in masses and spin for typical observations (small tidal deformability and signal-to-noise ratio ∼ 25). However, with increasing signal-to-noise ratio or tidal deformability there are biases in the estimates of the binary parameters. The post-merger regime, instead, has no impact on gravitational-wave measurements with current detectors for the signal-to-noise ratios we consider.PACS numbers: 04.25.D-, 95.30.Sf

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Stillen beeinträchtigt/Stillen erfolgreich

Cited by 2 publications

References 0 publications

Oscillations of rapidly rotating relativistic stars

Oscillations of rapidly rotating relativistic stars

Relevance of tidal effects and post-merger dynamics for binary neutron star parameter estimation

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