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

By K. Kotake, Katsuhiko Sato, Keitaro Takahashi. 2005

248 citations recorded by the source corpus.

Core-collapse supernovae are among the most energetic explosions in the universe marking the catastrophic end of massive stars. In spite of rigorous studies for several decades, we still do not understand the explosion mechanism completely. Since they are related to many astrophysical phenomena such as nucleosynthesis, gamma-ray bursts and acceleration of cosmic rays, understanding of their physics has been of wide interest to the astrophysical community. In this paper, we review recent progress in the study of core-collapse supernovae focusing on the explosion mechanism, supernova neutrinos and the gravitational waves. Regarding the explosion mechanism, we present a review paying particular attention to the roles of multidimensional aspects, such as convection, rotation and magnetic fields, on the neutrino heating mechanism. Next, we discuss supernova neutrino, which is a powerful tool to probe not only deep inside the supernovae but also the intrinsic properties of neutrinos. For this purpose, it is necessary to understand neutrino oscillation which has been established recently by many experiments. Gravitational astronomy is also now becoming a reality. We present an extensive review on the physical foundations and the emission mechanism of gravitational waves in detail and discuss the possibility of their detections.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/64b85b949699eaed7aee639a5e199717060e69fd

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Citations in the corpus

Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “Thus they are good candidates for sizable gravitational-wave pulses from the moment of core bounce (e.g., Kotake et al. 2006; Ott et al. 2004).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, background): “…strong magnetic fields require very rapid rotation that may not be available in the generic core-collapse supernova context (Ott et al. 2006a), magnetic jets have been suggested as potential power sources (Akiyama et al. 2003; Kotake et al. 2006; Moiseenko et al. 2006; Obergaulinger et al. 2006).”
IceCube sensitivity for low-energy neutrinos from nearby supernovae (2011, background): “With just 24neutrinos collected, stringent limits on the mass of the ¯νe, its lifetime, its magnetic moment and the number of leptonic flavors could be derived (Kotake et al., 2006).”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, background): “ck-hole and neutron star binaries (e.g., [16, 17, 18]), neutron star normal mode oscillations (e.g., [19]), rotating neutron star mountains (e.g., [20]), and core-collapse supernova explosions (e.g., [21, 22, 23] for recent reviews), on the ﬁnal of which w e focus in this article. According to the E”
THE COSMIC CORE-COLLAPSE SUPERNOVA RATE DOES NOT MATCH THE MASSIVE-STAR FORMATION RATE (2011, background): “…densities and temperatures reached in CC SNe offer the opportunity to study the physics of weakly interacting particles, formation of compact objects, and related nuclear physics (see, e.g., Raffelt 1990, 2000; Kotake et al. 2006; Janka et al. 2007; Lattimer & Prakash 2007, for recent reviews).”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, background): “…as the acoustic mechanism (e.g., Burrows et al. (2006)) or the magnetohydrodynamic mechanism (e.g., Kotake et al. (2004); Takiwaki et al. (2004, 2009); Burrows et al. (2007a); Guilet et al. (2010); Obergaulinger & Janka (2011);?, see also Kotake et al. (2006) for collective references therein).”
Gravitational-wave sensitivity curves (2014, background): “Simulations of core-collapse supernovae show that GWs between (102– 103) Hz can be produced (Kotake et al 2006).”
THE ISOTROPIC DIFFUSION SOURCE APPROXIMATION FOR SUPERNOVA NEUTRINO TRANSPORT (2007, background): “…spatial dimensions, for example the pattern of the accretion flow (Herant et al. 1994), the standing accretion shock instability (Blondin et al. 2003), the excitation of PNS g-modes (Burrows et al. 2006), and the evolution of magnetic fields (see e.g. Kotake et al. (2006) and references therein).”