SASI in Three Dimensions

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Model

To study the evolution of the SASI in three dimensions we follow the the simulations described in Blondin & Mezzacappa (2006) in which the stalled supernova shock is modeled as a spherical accretion shock above a hard, reflecting boundary. The location of the stationary shock is controlled by the magnitude of optically-thin cooling in a thin layer above the surface of the accreting star (the proto-neutron star).

Geometry

The present work extends the numerical studies of Blondin & Mezzacappa (2006) to three dimensions using the Yin-Yang overset spherical grid geometry. This approach retains the ability to fully resolve the thin, spherical cooling layer at the surface of the star.

Procedure

The SASI is excited by dropping a density perturbation onto the shock. The growth of the SASI modes is measured by tracking the Fourier components of the angular velocity.