Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae
Naofumi Ohnishi, Kei Kotake, Shoichi Y. Amada
ENG - Aerospace Engineering
We present the results of numerical experiments, in which we have investigated the influence of the inelastic neutrino-helium interactions on the standing accretion shock instability supposed to occur in the postbounce supernova core. The axisymmetric hydrodynamical simulations of accretion flows through the standing accretion shock wave onto the proto-neutron star show that the interactions are relatively minor and the linear growth of the shock instability is hardly affected. The extra heating given by the inelastic reactions becomes important for the shock revival after the instability enters the nonlinear regime, but only when the neutrino luminosity is very close to the critical value at which the shock would be revived without the interactions. We have also studied the dependence of the results on the initial amplitudes of perturbation and the temperatures of mu and tau neutrinos.
Instabilities
Neutrinos
Supernovae: general
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helium Earth & Environmental Sciences
supernovae Physics & Astronomy
neutrinos Physics & Astronomy
shock Physics & Astronomy
shock wave Earth & Environmental Sciences
Ohnishi, N., Kotake, K., & Amada, S. Y. (2007). Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae. Astrophysical Journal, 667(1 I), 375-381. https://doi.org/10.1086/520755
Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae. / Ohnishi, Naofumi; Kotake, Kei; Amada, Shoichi Y.
In: Astrophysical Journal, Vol. 667, No. 1 I, 2007, p. 375-381.
Ohnishi, N, Kotake, K & Amada, SY 2007, 'Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae', Astrophysical Journal, vol. 667, no. 1 I, pp. 375-381. https://doi.org/10.1086/520755
Ohnishi N, Kotake K, Amada SY. Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae. Astrophysical Journal. 2007;667(1 I):375-381. https://doi.org/10.1086/520755
Ohnishi, Naofumi ; Kotake, Kei ; Amada, Shoichi Y. / Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae. In: Astrophysical Journal. 2007 ; Vol. 667, No. 1 I. pp. 375-381.
@article{2cdcc5f382fd4e70bcd875f9ca8f8c56,
title = "Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae",
abstract = "We present the results of numerical experiments, in which we have investigated the influence of the inelastic neutrino-helium interactions on the standing accretion shock instability supposed to occur in the postbounce supernova core. The axisymmetric hydrodynamical simulations of accretion flows through the standing accretion shock wave onto the proto-neutron star show that the interactions are relatively minor and the linear growth of the shock instability is hardly affected. The extra heating given by the inelastic reactions becomes important for the shock revival after the instability enters the nonlinear regime, but only when the neutrino luminosity is very close to the critical value at which the shock would be revived without the interactions. We have also studied the dependence of the results on the initial amplitudes of perturbation and the temperatures of mu and tau neutrinos.",
keywords = "Hydrodynamics, Instabilities, Neutrinos, Supernovae: general",
author = "Naofumi Ohnishi and Kei Kotake and Amada, {Shoichi Y.}",
T1 - Inelastic neutrino-helium scatterings and standing accretion shock instability in core-collapse supernovae
AU - Ohnishi, Naofumi
AU - Kotake, Kei
AU - Amada, Shoichi Y.
N2 - We present the results of numerical experiments, in which we have investigated the influence of the inelastic neutrino-helium interactions on the standing accretion shock instability supposed to occur in the postbounce supernova core. The axisymmetric hydrodynamical simulations of accretion flows through the standing accretion shock wave onto the proto-neutron star show that the interactions are relatively minor and the linear growth of the shock instability is hardly affected. The extra heating given by the inelastic reactions becomes important for the shock revival after the instability enters the nonlinear regime, but only when the neutrino luminosity is very close to the critical value at which the shock would be revived without the interactions. We have also studied the dependence of the results on the initial amplitudes of perturbation and the temperatures of mu and tau neutrinos.
AB - We present the results of numerical experiments, in which we have investigated the influence of the inelastic neutrino-helium interactions on the standing accretion shock instability supposed to occur in the postbounce supernova core. The axisymmetric hydrodynamical simulations of accretion flows through the standing accretion shock wave onto the proto-neutron star show that the interactions are relatively minor and the linear growth of the shock instability is hardly affected. The extra heating given by the inelastic reactions becomes important for the shock revival after the instability enters the nonlinear regime, but only when the neutrino luminosity is very close to the critical value at which the shock would be revived without the interactions. We have also studied the dependence of the results on the initial amplitudes of perturbation and the temperatures of mu and tau neutrinos.
KW - Hydrodynamics
KW - Instabilities
KW - Neutrinos
KW - Supernovae: general