Stochastic Nature of Gravitational Waves From Supernova Explosions With Standing Accretion Shock Instability

Kotake, Kei; Iwakami, Wakana; Ohnishi, Naofumi; Yamada, Shoichi

doi:10.1088/0004-637x/697/2/l133

Cited by 91 publications

(130 citation statements)

References 39 publications

(40 reference statements)

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“…Hayama et al [73] studied the detectability of GWs from multidimensional CCSN simulations from [38,[74][75][76]. Using the coherent network analysis network pipeline RIDGE [77], signals in simulated Gaussian noise for a four-detector network containing the two Advanced LIGO detectors, Advanced Virgo, and KAGRA are considered.…”

Section: Introductionmentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5 kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

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Section: Introductionmentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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“…Several authors also investigated the influence of magnetic fields on the GW signal during the collapse and early post-bounce evolution assuming axisymmetry (Kotake et al 2004;Yamada & Sawai 2004;Kotake et al 2005;Obergaulinger et al 2006a,b) and no symmetry restriction at all (Scheidegger et al 2008(Scheidegger et al , 2010. The GW signal caused by aspherical neutrino emission was first studied by Epstein (1978) and subsequently by Burrows & Hayes (1996), Müller & Janka (1997), and Kotake et al (2007Kotake et al ( , 2009aKotake et al ( ,b, 2011, where the investigations by Müller & Janka (1997) and Kotake et al (2009bKotake et al ( , 2011 considered also 3D, i.e., non-axisymmetric models.…”

Section: Introductionmentioning

confidence: 99%

“…Gravitational wave emission occurs owing to matter asymmetries that arise from perturbations caused by precollapse convection, core rotation, and low-mode convection in the explosion engine itself, and owing to anisotropic neutrino emission. Kotake et al (2009b) simulated 3D mock-up models that mimic neutrino-driven explosions aided by the SASI, and computed the GW signal resulting from anisotropic neutrino emission by means of a ray-tracing method in a post-processing step. They pointed out that the gravitational waveforms of 3D models vary much more stochastically than those of axisymmetric ones, i.e., in 3D the GW signals do not possess any template character.…”

Section: Introductionmentioning

confidence: 99%

Parametrized 3D models of neutrino-driven supernova explosions

Müller

Janka

Wongwathanarat

2012

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Time-dependent and direction-dependent neutrino and gravitational-wave (GW) signatures are presented for a set of three-dimensional (3D) hydrodynamic models of parametrized, neutrino-driven supernova explosions of non-rotating 15 and 20 M stars. We employed an approximate treatment of neutrino transport based on a gray spectral description and a ray-by-ray treatment of multi-dimensional effects. Owing to the excision of the high-density core of the proto-neutron star (PNS) and the use of an axis-free (Yin-Yang) overset grid, the models can be followed from the post-bounce accretion phase through the onset of the explosion into more than one second of the early cooling evolution of the PNS without imposing any symmetry restrictions and covering a full sphere. Gravitational waves and neutrino emission exhibit the generic time-dependent features already known from 2D (axi-symmetric) models. Violent non-radial hydrodynamic mass motions in the accretion layer and their interaction with the outer layers of the proto-neutron star together with anisotropic neutrino emission give rise to a GW signal with an amplitude of ∼5−20 cm in the frequency range of 100−500 Hz. The GW emission from mass motions usually reaches a maximum before the explosion sets in. After the onset of the explosion the GW signal exhibits a low-frequency modulation, in some cases describing a quasi-monotonic growth, associated with the non-spherical expansion of the explosion shock wave and the large-scale anisotropy of the escaping neutrino flow. Variations of the mass-quadrupole moment caused by convective activity inside the nascent neutron star add a high-frequency component to the GW signal during the post-explosion phase. The GW signals exhibit strong variability between the two polarizations, different explosion simulations and different observer directions, and besides common basic features do not possess any template character. The neutrino emission properties (fluxes and effective spectral temperatures) show fluctuations over the neutron star surface on spatial and temporal scales that reflect the different types of non-spherical mass motions in the supernova core, i.e., post-shock overturn flows and proto-neutron star convection. However, because very prominent, quasi-periodic sloshing motions of the shock caused by the standing accretion-shock instability are absent and the emission from different surface areas facing an observer adds up incoherently, the modulation amplitudes of the measurable neutrino luminosities and mean energies are significantly lower than predicted by 2D simulations.

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“…A multitude of GW emission processes may be active in the postbounce, pre-explosion phase. These include convection/turbulence in the protoneutron star and in the postshock region, nonaxisymmetric rotational instabilities of the protoneutron star, protoneutron star pulsations, instabilities of the standing accretion shock, and asymmetric emission of neutrinos ( [3,[12][13][14][15][16] and references therein).…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave extraction in simulations of rotating stellar core collapse

et al. 2011

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We perform simulations of general relativistic rotating stellar core collapse and compute the gravitational waves (GWs) emitted in the core bounce phase of three representative models via multiple techniques. The simplest technique, the quadrupole formula (QF), estimates the GW content in the spacetime from the mass quadrupole tensor only. It is strictly valid only in the weakfield and slow-motion approximation. For the first time, we apply GW extraction methods in core collapse that are fully curvature-based and valid for strongly radiating and highly relativistic sources. These techniques are not restricted to weak-field and slow-motion assumptions. We employ three extraction methods computing (i) the Newman-Penrose (NP) scalar Ψ4, (ii) Regge-Wheeler-ZerilliMoncrief (RWZM) master functions, and (iii) Cauchy-Characteristic Extraction (CCE) allowing for the extraction of GWs at future null infinity, where the spacetime is asymptotically flat and the GW content is unambiguously defined. The latter technique is the only one not suffering from residual gauge and finite-radius effects. All curvature-based methods suffer from strong non-linear drifts. We employ the fixed-frequency integration technique as a high-pass waveform filter. Using the CCE results as a benchmark, we find that finite-radius NP extraction yields results that agree nearly perfectly in phase, but differ in amplitude by ∼ 1 − 7% at core bounce, depending on the model. RWZM waveforms, while in general agreeing in phase, contain spurious high-frequency noise of comparable amplitudes to those of the relatively weak GWs emitted in core collapse. We also find remarkably good agreement of the waveforms obtained from the QF with those obtained from CCE. The results from QF agree very well in phase and systematically underpredict peak amplitudes by ∼ 5−11%, which is comparable to the NP results and is certainly within the uncertainties associated with core collapse physics.

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Stochastic Nature of Gravitational Waves From Supernova Explosions With Standing Accretion Shock Instability

Cited by 91 publications

References 39 publications

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Parametrized 3D models of neutrino-driven supernova explosions

Gravitational wave extraction in simulations of rotating stellar core collapse

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