Gravitational waves from core collapse supernovae

Yakunin, Konstantin N.; Marronetti, Pedro; Mezzacappa, Anthony; Bruenn, Stephen W.; Lee, Ching-Tsai; Chertkow, Merek A.; Hix, W. R.; Blondin, John M.; Lentz, Eric J.; Messer, O. E. Bronson; Yoshida, Shin’ichirou

doi:10.1088/0264-9381/27/19/194005

Cited by 156 publications

(138 citation statements)

References 24 publications

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“…The gravitational wave emission also exhibits the generic time-dependent features already known from 2D (axisymmetric) models, but the 3D wave amplitudes are considerably lower (by a factor of 2−3) than those predicted by 2D models (Müller et al 2004;Murphy et al 2009;Yakunin et al 2010) owing to less coherent mass motions and neutrino emission. Note in this respect that the GW quadrupole amplitudes, which are usually quoted for 2D models (A E2 20 ), have to be multiplied by a geometric factor sin 2 θ √ 15/π/8 (which is equal to ≈0.27 for θ = 90 • ).…”

Section: Discussionmentioning

confidence: 67%

“…Later on, sizable g-mode activity is instigated in the outer layers of the proto-neutron star by convective overturn and the SASI during the hydrodynamically vigorous pre-explosion phase, and by the impact of anisotropic accretion flows during the subsequent post-explosion accretion phase ). This g-mode activity is the cause of GW signals Murphy et al 2009;Yakunin et al 2010), whose maximum amplitudes are on the order of a few centimeters centered around zero.…”

Section: Resultsmentioning

confidence: 99%

“…However, most studies of the past thirty years were either concerned with the collapse and bounce signal only (Müller 1982;Finn & Evans 1990;Mönchmeyer et al 1991;Yamada & Sato 1994;Zwerger & Müller 1997;Rampp et al 1998;Dimmelmeier et al 2001Dimmelmeier et al , 2002Kotake et al 2003;Shibata 2003;Shibata & Sekiguchi 2004;Ott et al 2004;Cerda-Duran et al 2005;Saijo 2005;Shibata & Sekiguchi 2005;Kotake et al 2006;Dimmelmeier et al 2007;Ott et al 2007;Dimmelmeier et al 2008), or were A&A 537, A63 (2012) restricted to axisymmetric (2D) models (Müller et al 2004;Ott et al 2006;Kotake et al 2007;Murphy et al 2009;Yakunin et al 2010). 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.…”

Section: Introductionmentioning

confidence: 99%

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Parametrized 3D models of neutrino-driven supernova explosions

Müller

Janka

Wongwathanarat

2012

A&A

113

144

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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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Section: Discussionmentioning

confidence: 67%

Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Parametrized 3D models of neutrino-driven supernova explosions

Müller

Janka

Wongwathanarat

2012

A&A

113

144

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“…A direct gravitational wave (GW) detection will open an alternative and complementary perspective on the Cosmos (Sathyaprakash & Schutz 2009). According to General Relativity, accelerating masses with a mass quadrupole moment varying in time generate GWs, and our Universe has plenty of systems fulfilling such a requirement (Wald 1983;Maggiore 2008); from compact binaries (emitting GWs while inspiraling towards one another until coalescence, Peters & Mathews 1963), to asymmetric spinning compact stars (Van Den Broeck 2005), and catastrophic supernovae explosions (Yakunin et al 2010), just to mention a few.…”

Section: Introductionmentioning

confidence: 99%

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Rosado

Sesana

Gair

2015

Monthly Notices of the Royal Astronomical Society

187

235

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In this paper we attempt to investigate the nature of the first gravitational wave (GW) signal to be detected by pulsar timing arrays (PTAs): will it be an individual, resolved supermassive black hole binary (SBHB), or a stochastic background made by the superposition of GWs produced by an ensemble of SBHBs? To address this issue, we analyse a broad set of simulations of the cosmological population of SBHBs, that cover the entire parameter space allowed by current electromagnetic observations in an unbiased way. For each simulation, we construct the expected GW signal and identify the loudest individual sources. We then employ appropriate detection statistics to evaluate the relative probability of detecting each type of source as a function of time for a variety of PTAs; we consider the current International PTA, and speculate into the era of the Square Kilometre Array. The main properties of the first detectable individual SBHBs are also investigated. Contrary to previous work, we cast our results in terms of the detection probability (DP), since the commonly adopted criterion based on a signal-to-noise ratio threshold is statistic-dependent and may result in misleading conclusions for the statistics adopted here. Our results confirm quantitatively that a stochastic signal is more likely to be detected first (with between 75 to 93 per cent probability, depending on the array), but the DP of single-sources is not negligible. Our framework is very flexible and can be easily extended to more realistic arrays and to signal models including environmental coupling and SBHB eccentricity.

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“…For a burst emission in the center of our Galaxy (∼10 kpc), these values allow a detect with 50% efficiency, if the sources emit an energy of about 2.2 × 10 −8 solar masses, a value not far from the prediction of the modern models of a supernova explosion [16,17].…”

Section: Ricap-2014mentioning

confidence: 87%

Gravitational waves and multimessenger astronomy

Ricci

2016

EPJ Web of Conferences

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Abstract. It is widely expected that in the coming quinquennium the first gravitational wave signal will be directly detected. The ground-based advanced LIGO and Virgo detectors are being upgraded to a sensitivity level such that we expect to be measure a significant binary merger rate. Gravitational waves events are likely to be accompanied by electromagnetic counterparts and neutrino emission carrying complementary information to those associated to the gravitational signals. If it becomes possible to measure all these forms of radiation in concert, we will end up an impressive increase in the comprehension of the whole phenomenon. In the following we summarize the scientific outcome of the interferometric detectors in the past configuration. Then we focus on some of the potentialities of the advanced detectors once used in the new context of the multimessenger astronomy.

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Gravitational waves from core collapse supernovae

Cited by 156 publications

References 24 publications

Parametrized 3D models of neutrino-driven supernova explosions

Parametrized 3D models of neutrino-driven supernova explosions

Expected properties of the first gravitational wave signal detected with pulsar timing arrays

Gravitational waves and multimessenger astronomy

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