Neutrino-driven convection versus advection in core collapse supernovae

TL;DR

This paper presents a simplified model to analyze the linear stability of the gain region behind a stalled shock in core-collapse supernovae, highlighting the role of advection and buoyancy in stability criteria.

Contribution

It introduces a new stability criterion based on the ratio of advection time to buoyancy timescale, and explores how this affects convection and asymmetries in supernova explosions.

Findings

Stability depends on the ratio ; gain region is stable if <3.

Classical convection occurs when ;3.

Long wavelength perturbations are stabilized by advection, affecting global asymmetries.

Abstract

A toy model is analyzed in order to evaluate the linear stability of the gain region immediately behind a stalled accretion shock, after core bounce. This model demonstrates that a negative entropy gradient is not sufficient to warrant linear instability. The stability criterion is governed by the ratio \chi of the advection time through the gain region divided by the local timescale of buoyancy. The gain region is linearly stable if \chi< 3. The classical convective instability is recovered in the limit \chi\gg 3. For \chi>3, perturbations are unstable in a limited range of horizontal wavelengths centered around twice the vertical size H of the gain region. The threshold horizontal wavenumbers k_{min} and k_{max} follow simple scaling laws such that Hk_{min}\propto 1/{\chi} and Hk_{max}\propto \chi. The convective stability of the l=1 mode in spherical accretion is discussed, in relation with the asymmetric explosion of core collapse supernovae. The advective stabilization of long wavelength perturbations weakens the possible influence of convection alone on a global l=1 mode.