Development of Structure in Supernova Simulations From the Explosion out to Late Times

Details Development of Structure in Supernova Simulations From the Explosion out to Late Times Development of Structure in Supernova Simulations From the Explosion out to Late Times

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21742305e&link_type=abstract

American Astronomical Society, AAS Meeting #217, #423.05; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Detailed and spatially resolved observations of supernova remnants suggest that early in the evolution of the remnant the SN ejecta fragments and forms over-dense knots (Spyromilio et al. 1993). Knots are also observed in the SNRs many years after the explosion (e.g. Moon et al. 2009, Ghavamian et al. 2005, Hammell & Fesen 2008).
We are currently doing numerical simulations of supernova explosions in three dimensions to study the fragmentation of supernova ejecta from the onset of the explosion. We are specifically interested in the formation and development of features like ejecta knots, their physical properties (size, mass, composition, temperature evolution), the factors that influence all those, and in assessing whether these are transient or long-lived features. For the calculations we are using a parallel, 3D Smooth Particle Hydrodynamics code (SNSPH, Fryer et al. 2006), with a small (20 isotope) nuclear reaction network and a radiative cooling routine.
We have performed a number of runs (a spherically symmetric explosion of a 15 Msol star with 1, 10, and 50 million SPH particles, a strong, spherically symmetric explosion of a 16 Msol simulated binary star with 1 and 50 million particles, and two different cases of bipolar explosions for those stars) that were evolved out to at least 1 yr. All scenarios of the 15 Msol explosions show the development of prominent, finger-like structures, that persist at least out to 20 yrs (the end of the longest calculation). These structures are likely due to Richtmyer-Meshkov instabilities that develop as the shock moves through the star. We will be presenting a comparison between the different runs, focusing on the effect of spatial resolution in the calculation, effect of asymmetry on development of structure and resulting altered nucleosynthesis, and effects of timing of adding an asymmetry on the developing structure.

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