The saturation of the Standing Accretion Shock Instability by parasitic instabilities

Details The saturation of the Standing Accretion Shock Instability by parasitic instabilities The saturation of the Standing Accretion Shock Instability by parasitic instabilities

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009sf2a.conf..157g&link_type=abstract

SF2A-2009: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, held 29 June - 4 July 2009 in

Astronomy and Astrophysics

Astrophysics

Scientific paper

The Standing Accretion Shock Instability (SASI) is commonly believed to be the cause of large amplitude dipolar shock oscillations observed in numerical simulations of the stalled shock phase of core collapse supernovae. We investigate the role of parasitic instabilities as a possible cause of nonlinear SASI saturation. As the shock oscillations create both vorticity and entropy gradients, we show that both Kelvin-Helmholtz and Rayleigh-Taylor types of instabilities are able to grow on a SASI mode if its amplitude is large enough. We obtain approximate formulae for their growth rates, taking into account the effects of advection and entropy stratification, and use them to estimate the saturation amplitude of SASI. When applied to the set up of Fernández & Thompson (2009), this saturation mechanism is able to explain the dramatic decrease of the SASI power when both the nuclear dissociation energy and the cooling rate are varied. Our results open new perspectives for anticipating the effects, on the SASI amplitude, of the physical ingredients involved in the model of the collapsing star.

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