Effect of Rotation on the Stability of a Stalled Cylindrical Shock and its Consequences for Core-Collapse Supernovae

TL;DR

This paper investigates how rotation influences the stability and growth of spiral modes in the SASI during core-collapse supernovae, highlighting the importance of 3D modeling for understanding explosion mechanisms.

Contribution

It provides a perturbative analysis showing rotation's impact on SASI modes, emphasizing the dominance of spiral modes aligned with flow rotation in supernovae.

Findings

Rotation increases growth rates of spiral modes aligned with flow

Counter-rotating modes are damped by rotation

Mode m=1 favored at low rotation, m=2 at higher rotation

Abstract

A perturbative analysis is used to investigate the effect of rotation on the instability of a steady accretion shock (SASI) in a simple toy-model, in view of better understanding supernova explosions in which the collapsing core contains angular momentum. A cylindrical geometry is chosen for the sake of simplicity. Even when the centrifugal force is very small, rotation can have a strong effect on the non axisymmetric modes of SASI by increasing the growth rate of the spiral modes rotating in the same direction as the steady flow. Counter-rotating spiral modes are significantly damped, while axisymmetric modes are hardly affected by rotation. The growth rates of spiral modes have a nearly linear dependence on the specific angular momentum of the flow. The fundamental one-armed spiral mode (m=1) is favoured for small rotation rates, whereas stronger rotation rates favour the mode m=2. A WKB analysis of higher harmonics indicates that the efficiency of the advective-acoustic cycles associated to spiral modes is strongly affected by rotation in the same manner as low frequency modes, whereas the purely acoustic cycles are stable. These results suggest that the linear phase of SASI in rotating core-collapse supernovae naturally selects a spiral mode rotating in the same direction of the flow, as observed in the 3D numerical simulations of Blondin & Mezzacappa (2007). This emphasizes the need for a 3D approach of rotating core-collapse, before conclusions on the explosion mechanisms and pulsar kicks can be drawn.