Spiral mode of standing accretion shock instability in core-collapse supernovae

Details Spiral mode of standing accretion shock instability in core-collapse supernovae Spiral mode of standing accretion shock instability in core-collapse supernovae

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ap%26ss.322...43i&link_type=abstract

Astrophysics and Space Science, Volume 322, Issue 1-4, pp. 43-47

Astronomy and Astrophysics

Astrophysics

3

Supernovae, Hydrodynamics, Instability

Scientific paper

The study of standing accretion shock instability (SASI) in core-collapse supernova cores has been done with three-dimensional (3D) computer simulations. Rotations with various perturbations were introduced from outer boundary of an initial steady accreting flow. We found that one or two armed spiral accreting flow onto the proto-neutron star (PNS) is formed inside the shock wave depending on perturbations. The linear growth of spiral modes are clearly diagnosed by the mode analysis of the shock surface, and the lower m modes grow quickly in the linear regime.

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