Critical Conditions for Core-Collapse Supernovae

Abstract

The explosion of a core-collapse supernova can be approximated by the breakdown of steady-state solutions for accretion onto a proto-neutron star (PNS). We analytically show that as the neutrino luminosity exceeds a critical value L_c, the neutrinosphere pressure exceeds the hydrostatic limit even for an optimal shock radius R. This yields L_c \propto M^2 T^2 (with logarithmic corrections) and R \propto M/T, in agreement with numerical results, where M, T are the PNS mass, neutrino temperature. The near-critical flow can be approximated as a ballistic shell on top of an isothermal layer.

PRL accepted

References in corpus (5)

• Theory of Core-Collapse Supernovae
• Dimension as a Key to the Neutrino Mechanism of Core-Collapse Supernova Explosions
• Criteria for Core-Collapse Supernova Explosions by the Neutrino Mechanism
• The Physics of the Neutrino Mechanism of Core-Collapse Supernovae
• 2D and 3D Core-Collapse Supernovae Simulation Results Obtained with the CHIMERA Code

Cited by in corpus (8)

• Explosion Mechanisms of Core-Collapse Supernovae
• What can be learned from a future supernova neutrino detection?
• The criterion of supernova explosion revisited: the mass accretion history
• Effects of rotation and magnetic field on the revival of a stalled shock in supernova explosions
• Semi-dynamical approach to the shock revival in core-collapse supernovae
• A Force Explosion Condition for Spherically Symmetric Core-collapse Supernovae
• Shock Revival in Core-Collapse Supernovae: A Phase-Diagram Analysis
• The Force Explosion Condition is Consistent with Spherically Symmetric CCSN Explosions