Explosion mechanism, neutrino burst and gravitational wave in core-collapse supernovae

Kotake, Kei; Sato, Katsuhiko; Takahashi, Keitaro

doi:10.1088/0034-4885/69/4/r03

Cited by 325 publications

(363 citation statements)

References 355 publications

(973 reference statements)

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“…The up to now only recorded neutrino signal of a core-collapse supernova (SN1987A) confirmed the idea that the collapse of the core of a massive star to neutron star densities provides the necessary energy for the explosion (Baade & Zwicky 1934). Because gravitational waves (GW), the only other means to probe the supernova engine besides neutrinos, are yet to be detected, supernova modelers are preparing for this prospective measurement by predicting the gravitational wave signature of core-collapse supernovae with ever increasing realism (for reviews, see e.g., Kotake et al 2006;Ott 2009;Fryer & New 2011).…”

Section: Introductionmentioning

confidence: 95%

“…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

125

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: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

Parametrized 3D models of neutrino-driven supernova explosions

Müller

Janka

Wongwathanarat

2012

A&A

125

144

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“…Various mechanisms for producing the asymmetry have been discussed, including convection (e.g., Herant et al 1994;Burrows et al 1995;Janka & Mueller 1996), magnetic field and rapid rotation (see, e.g., Kotake et al 2006 for collective references), standing (stationary, spherical) accretion shock instability, or SASI ( Blondin et al 2003;Scheck et al 2004;Blondin & Mezzacappa 2006;Ohnishi et al 2006Ohnishi et al , 2007Foglizzo et al 2006), and g-mode oscillations of protoYneutron stars ( Burrows et al 2006). Most of these, however, have been investigated only with two-dimensional (2D) simulations.…”

Section: Introductionmentioning

confidence: 99%

Three‐Dimensional Simulations of Standing Accretion Shock Instability in Core‐Collapse Supernovae

Iwakami

Kotake

Ohnishi

et al. 2008

ApJ

Self Cite

137

218

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We have studied nonaxisymmetric standing accretion shock instabilities, or SASI, using three-dimensional (3D) hydrodynamical simulations. This is an extension of our previous study of axisymmetric SASI. We have prepared a spherically symmetric and steady accretion flow through a standing shock wave onto a protoYneutron star, taking into account a realistic equation of state and neutrino heating and cooling. This unperturbed model is meant to represent approximately the typical postbounce phase of core-collapse supernovae. We then added a small perturbation ($1%) to the radial velocity and computed the ensuing evolutions. Both axisymmetric and nonaxisymmetric perturbations have been imposed. We have applied mode analysis to the nonspherical deformation of the shock surface, using spherical harmonics. We have found that (1) the growth rates of SASI are degenerate with respect to the azimuthal index m of the spherical harmonics Y m l , just as expected for a spherically symmetric background; (2) nonlinear mode couplings produce only m ¼ 0 modes for axisymmetric perturbations, whereas m 6 ¼ 0 modes are also generated in the nonaxisymmetric cases, according to the selection rule for quadratic couplings; (3) the nonlinear saturation level of each mode is lower in general for 3D than for 2D, because a larger number of modes contribute to turbulence in 3D; (4) low-l modes are dominant in the nonlinear phase; (5) equipartition is nearly established among different m modes in the nonlinear phase; (6) spectra with respect to l obey power laws with a slope slightly steeper for 3D; and (7) although these features are common to the models with and without a shock revival at the end of the simulation, the dominance of low-l modes is more remarkable in the models with a shock revival.

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“…In Fe-core supernovae shock effects appear at much later times. Below we illustrate these effects in detail and compare them to the results for Fe-core supernovae from the literature (e.g., [24,33,34]). In our calculations we have used the results of Duan et al [7] for the pre-shock phase, and the density profiles in fig.…”

Section: A Probabilitiesmentioning

confidence: 88%

“…Here we review them briefly, in the measure needed to highlight the phenomena that are distinctive of a ONeMg-core supernova. We refer to the literature for more complete reviews (e.g., [24,33,34]). …”

Section: Flavor Conversion In the Star And In The Earth: Generalmentioning

confidence: 99%

Neutrino oscillation signatures of oxygen-neon-magnesium supernovae

2008

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We discuss the flavor conversion of neutrinos from core collapse supernovae that have oxygenneon-magnesium (ONeMg) cores. Using the numerically calculated evolution of the star up to 650 ms post bounce, we find that, for the normal mass hierarchy, the electron neutrino flux in a detector shows signatures of two typical features of an ONeMg-core supernova: a sharp step in the density profile at the base of the He shell and a faster shock wave propagation compared to iron core supernovae. Before the shock hits the density step (t < ∼ 150 ms), the survival probability of electron neutrinos above ∼20 MeV of energy is about ∼ 0.68, in contrast to values of ∼ 0.32 or less for an iron core supernova. The passage of the shock through the step and its subsequent propagation cause a decrease of the survival probability and a decrease of the amplitude of oscillations in the Earth, reflecting the transition to a more adiabatic propagation inside the star. These changes affect the lower energy neutrinos first; they are faster and more sizable for larger θ13. They are unique of ONeMg-core supernovae, and give the possibility to test the speed of the shock wave. The time modulation of the Earth effect and its negative sign at the neutronization peak are the most robust signatures in a detector.

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Explosion mechanism, neutrino burst and gravitational wave in core-collapse supernovae

Cited by 325 publications

References 355 publications

Parametrized 3D models of neutrino-driven supernova explosions

Parametrized 3D models of neutrino-driven supernova explosions

Three‐Dimensional Simulations of Standing Accretion Shock Instability in Core‐Collapse Supernovae

Neutrino oscillation signatures of oxygen-neon-magnesium supernovae

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