Formation and Initial Evolution of Rayleigh-Taylor Clumps in the Ejecta of Supernova Simulations

Details Formation and Initial Evolution of Rayleigh-Taylor Clumps in the Ejecta of Supernova Simulations Formation and Initial Evolution of Rayleigh-Taylor Clumps in the Ejecta of Supernova Simulations

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21920302e&link_type=abstract

American Astronomical Society, AAS Meeting #219, #203.02

Astronomy and Astrophysics

Astronomy

Scientific paper

Theoretical stability considerations and detailed numerical simulations have shown that Rayleigh-Taylor (RT) instabilities arise in a core-collapse supernova (SN) shortly after the explosion, leading to the early fragmentation of some regions in the ejecta. The clumps thus created are of interest to a variety of topics, for example delivery of material to the surrounding interstellar medium or comparison to SN remnant features like the Cassiopeia A ejecta knots. One particular interest to the authors in the former of those topics is delivery of SN material to forming planetary systems, our solar system in particular, since there is evidence that the solar system was contaminated with SN debris shortly before or during its birth. Knowledge of isotopic information and the full thermodynamic evolution of such overdense clumps is of interest to this topic, but only partially obtainable from observations. Thus it would be useful to be able to assess the physical properties of structures that form in the SN ejecta. Numerical simulations of the explosions of core collapse supernovae were done in 3 dimensions to study the formation of overdense clumps. The calculations were done with a particle- based hydrodynamics code and followed out to at least 0.5 yrs after the explosion. It is found that RT instabilities result in clumps in the He- and C+O rich regions in the exploding star that are overdense by 1-2 orders of magnitude and typically a few percent of the expanding ejecta size in diameter. These RT clumps are expected to be related to the ejecta knots of the type observed in the Cassiopeia A supernova remnant, probably evolving into them in the subsequent expansion. Further calculations to study the interaction of the expanding ejecta with appropriate surrounding media and to follow the further evolution of the RT clumps are underway.

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