Oxygen-burning hydrodynamics. I. Steady shell burning

Research output: Contribution to journalArticle

28 Scopus citations

Abstract

With new hydrodynamic techniques, the relatively fast evolutionary stages of a star prior to core collapse may be explicitly computed in two spatial dimensions, with a treatment of the microphysics (e.g., nuclear reactions, equation of state, neutrino cooling) which is comparable to typical one-dimensional simulations. The nature of shell oxygen burning in a massive star, prior to core collapse, is used as a first example; it is of particular interest because it is (1) the region in which 56Ni will be produced by the supernova shock, (2) the region of the "mass cut," which will separate the collapsed core from the ejected mantle, (3) the site of much of the explosive nucleosynthesis, and (4) a suggested source of symmetry breaking to drive mixing instabilities which were observed in SN 1987A. The nature of the shell burning affects the size of the core which will collapse. The method is illustrated on this test case, and the character of the convection is examined.

Original languageEnglish (US)
Pages (from-to)932-946
Number of pages15
JournalAstrophysical Journal
Volume427
Issue number2
DOIs
StatePublished - Jun 1 1994

Keywords

  • Hydrodynamics
  • Nuclear reactions, nucleosynthesis, abundances
  • Supernova: general

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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