  By adding a weak magnetic field to a spherically symmetric fluid
configuration that caricatures a stalled shock in the post-bounce supernova
environment, we explore the capacity of the stationary accretion shock
instability (SASI) to generate magnetic fields. The SASI develops upon
perturbation of the initial condition, and the ensuing flow generates--{\em in
the absence of rotation}--dynamically significant magnetic fields ($\sim
10^{15}$ G) on a time scale that is relevant for the explosion mechanism of
core-collapse supernovae. We describe our model, present some recent results,
and discuss their potential relevance for supernova models.
