Si, O, Ne, and C shell burning

Casey Meakin, David Arnett

Research output: Contribution to journalArticlepeer-review


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.

Original languageEnglish (US)
Pages (from-to)296-297
Number of pages2
JournalProceedings of the International Astronomical Union
Issue numberS239
StatePublished - Aug 2006


  • Convection
  • Methods: numerical
  • Neutrinos
  • Nucleosynthesis
  • Stars: evolution
  • Stars: supernovae
  • Turbulence
  • Waves

ASJC Scopus subject areas

  • Medicine (miscellaneous)
  • Astronomy and Astrophysics
  • Nutrition and Dietetics
  • Public Health, Environmental and Occupational Health
  • Space and Planetary Science


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