Gravitational waves from rotating proto-neutron stars

Ferrari, Valeria; Gualtieri, Leonardo; Pons, José A.; Stavridis, Adamantios

doi:10.1088/0264-9381/21/5/019

Cited by 10 publications

(9 citation statements)

References 27 publications

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“…Additionally, the stratified structure of the PNS allows for the presence of different types of g-modes related to the fluid core [23]. Many subsequent works used simplified neutron star models assuming an equilibrium configuration as a background, to study the effect of rotation [24], general relativity [25], non-linearities [26], phase transitions [27] and realistic equation of state [28]. Only recently, there have been efforts to incorporate more suitable backgrounds based on numerical simulations in the computation of the mode structure and evolution [1,[29][30][31][32][33][34][35][36].…”

Section: Introductionmentioning

confidence: 99%

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

et al. 2021

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The eventual detection of gravitational waves from core-collapse supernovae (CCSN) will help improve our current understanding of the explosion mechanism of massive stars. The stochastic nature of the late post-bounce gravitational wave signal due to the non-linear dynamics of the matter involved and the large number of degrees of freedom of the phenomenon make the source parameter inference problem very challenging. In this paper we take a step towards that goal and present a parameter estimation approach which is based on the gravitational waves associated with oscillations of proto-neutron stars (PNS). Numerical simulations of CCSN have shown that buoyancy-driven g-modes are responsible for a significant fraction of the gravitational wave signal and their time-frequency evolution is linked to the physical properties of the compact remnant through universal relations, as demonstrated in [1]. We use a set of 1D CCSN simulations to build a model that relates the evolution of the PNS properties with the frequency of the dominant g-mode, which is extracted from the gravitational-wave data using a new algorithm we have developed for our study. The model is used to infer the time evolution of a combination of the mass and the radius of the PNS. The performance of the method is estimated employing simulations of 2D CCSN waveforms covering a progenitor mass range between 11 and 40 solar masses and different equations of state. Considering signals embedded in Gaussian gravitational wave detector noise, we show that it is possible to infer PNS properties for a galactic source using Advanced LIGO and Advanced Virgo data at design sensitivities. Third generation detectors such as Einstein Telescope and Cosmic Explorer will allow to test distances of O(100 kpc).

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Section: Introductionmentioning

confidence: 99%

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

et al. 2021

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“…The relation between É ðoÞ and the odd-parity metric multipoles is given, for example, by Eqs. (19)- (20) of Ref. [32].…”

Section: Perturbation Equationsmentioning

confidence: 99%

“…Although most of the work in perturbation theory has been done (and is still done) using a frequency-domain approach (in order to accurately compute mode frequencies), time-domain simulations are also needed to compute full waveforms [11][12][13][14][15][16][17][18][19][20][21][22][23]. In particular, Allen et al [12], via a multipolar expansion, derived the equations for the evenparity perturbations of spherically symmetric relativistic stars and produced explicit waveforms.…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves from pulsations of neutron stars described by realistic equations of state

Bernuzzi

Nagar

2008

Phys. Rev. D

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In this work we discuss the time evolution of nonspherical perturbations of a nonrotating neutron star described by a realistic equation of state (EOS). We analyze 10 different EOS for a large sample of neutron star models. Various kinds of generic initial data are evolved and the gravitational signals are computed. We focus on the dynamical excitation of fluid and spacetime modes and extract the corresponding frequencies. We employ a constrained numerical algorithm based on standard finitedifferencing schemes which permits stable and long-term evolutions. Our code provides accurate waveforms and allows one to capture, via Fourier analysis, the frequencies of the fluid modes with an accuracy comparable to that of frequency-domain calculations. The results we present here are useful for providing comparisons with simulations of nonlinear oscillations of (rotating) neutron star models as well as test beds for 3D nonlinear codes.

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“…No attempts have been made so far to estimate the GW signature during this phase, the main reason being the difficulty to perform multidimensional simulations of the PNS in such long time-scales, due to the severe time-step restrictions of numerical hydrodynamics codes. Ferrari et al (2003Ferrari et al ( , 2004Ferrari et al ( , 2007 have studied the appearance of unstable g-modes in PNSs as a possible source of GW, concluding that non-linear saturation would likely limit the maximum strain to values unobservable with current detectors. Very recently there has been an increased interest in the study of proto-neutron star convection (Nagakura et al 2020) and its associated dynamo (Raynaud et al 2020;Masada et al 2020), though these works have been focused on the early post-bounce phase and did not provide a description of the late-time post-explosion phase several seconds after bounce.…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave signature of proto-neutron star convection: I. MHD numerical simulations

Raynaud,

Cerdá-Durán,

Guilet

2021

Preprint

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Gravitational waves provide a unique and powerful opportunity to constrain the dynamics in the interior of proto-neutron stars during core collapse supernovae. Convective motions play an important role in generating neutron stars magnetic fields, which could explain magnetar formation in the presence of fast rotation. We compute the gravitational wave emission from protoneutron star convection and its associated dynamo, by post-processing three-dimensional MHD simulations of a model restricted to the convective zone in the anelastic approximation. We consider two different proto-neutron star structures representative of early times (with a convective layer) and late times (when the star is almost entirely convective). In the slow rotation regime, the gravitational wave emission follows a broad spectrum peaking at about three times the turnover frequency. In this regime, the inclusion of magnetic fields slightly decreases the amplitude without changing the spectrum significantly compared to a non-magnetised simulation. Fast rotation changes both the amplitude and spectrum dramatically. The amplitude is increased by a factor of up to a few thousands. The spectrum is characterized by several peaks associated to inertial modes, whose frequency scales with the rotation frequency. Using simple physical arguments, we derive scalings that reproduce quantitatively several aspects of these numerical results. We also observe an excess of low-frequency gravitational waves, which appears at the transition to a strong field dynamo characterized by a strong axisymmetric toroidal magnetic field. This signature of dynamo action could be used to constrain the dynamo efficiency in a proto-neutron star with future gravitational wave detections.

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Gravitational waves from rotating proto-neutron stars

Cited by 10 publications

References 27 publications

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

Inference of protoneutron star properties from gravitational-wave data in core-collapse supernovae

Gravitational waves from pulsations of neutron stars described by realistic equations of state

Gravitational wave signature of proto-neutron star convection: I. MHD numerical simulations

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