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Si, O, Ne, and C shell burning

Published online by Cambridge University Press:  01 August 2006

Casey Meakin  and
David Arnett
Casey Meakin
Affiliation:
Steward Observatory, University of Arizona, Tucson AZ 85721, USA email: [email protected]
David Arnett
Affiliation:
Steward Observatory, University of Arizona, Tucson AZ 85721, USA email: [email protected]
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Abstract

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We simulate the reactive-hydrodynamic flow for a variety of convective shell burning epochs in supernova progenitor models. The neutrino-cooled stages of carbon, neon, oxygen, and silicon burning are simulated in two and three dimensions. Even in the absence of rotation significant symmetry breaking occurs (10% in rms variation in thermodynamic variables such as temperature and density). These distortions are caused by turbulent convection interacting with stably stratified boundaries. Strong interactions of multiple active shells is seen; it is mediated by waves generated by convection. Some implications for supernova progenitors are presented.

Keywords

Convectionnucleosynthesisneutrinosturbulencewavesmethods: numericalstars: evolutionstars: supernovae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 296 - 297
Copyright
Copyright © International Astronomical Union 2007

References

Arnett, D. 1996, Supernovae and Nucleosynthesis, Princeton University Press, PrincetonCrossRefGoogle Scholar
Meakin, C. & Arnett, D. 2006a, “Active Carbon and Oxygen Burning Hydrodynamics”, ApJ 637, 53CrossRefGoogle Scholar
Meakin, C. & Arnett, D. 2006b, “Anelastic and Compressible Simulations of Stellar Oxygen Burning”, ApJ, submitted, astro-ph/0611317Google Scholar
Meakin, C. & Arnett, D. 2006c, “Turbulent Convection in Stellar Interiors: I. Hydrodynamic Simulations:, ApJ, submitted, astro-ph/0611315Google Scholar