Stability of the Accretion Flows with Stalled Shocks in Core-Collapse Supernovae

Details Stability of the Accretion Flows with Stalled Shocks in Core-Collapse Supernovae Stability of the Accretion Flows with Stalled Shocks in Core-Collapse Supernovae

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..937..344y&link_type=abstract

SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP Conference Proceedings, Volume 937, pp. 344-348 (2007).

Physics

Supernovae, Supernova Remnants, Accretion And Accretion Disks, Neutron Stars

Scientific paper

With an eye toward application to the theory of core-collapse supernovae, we performed a global linear analysis on the stability of spherically symmetric accretion flows through a standing shock wave onto a proto neutron star. We solved the equations for linear perturbations numerically, and obtained the eigen frequencies and eigen functions. The results show that the non-radial instabilities are induced, probably via the advection-acoustic cycles, for relatively low neutrino luminosities, e.g. ~2-7×1052 ergs/s for M = 1.0Msolar/s. For still larger luminosities, more than about 7×1052 ergs/s for the same accretion rate, non-oscillatory modes become unstable. These non-radial modes were identified as convection.

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