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Titolo:
OXYGEN-BURNING HYDRODYNAMICS .1. STEADY SHELL BURNING
Autore:
ARNETT D;
Indirizzi:
UNIV ARIZONA,STEWARD OBSERV TUCSON AZ 85721
Titolo Testata:
The Astrophysical journal
fascicolo: 2, volume: 427, anno: 1994,
parte:, 1
pagine: 932 - 946
SICI:
0004-637X(1994)427:2<932:OH.SSB>2.0.ZU;2-B
Fonte:
ISI
Lingua:
ENG
Soggetto:
MASSIVE STARS; EVOLUTION; CONVECTION;
Keywords:
HYDRODYNAMICS; NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; SUPERNOVA, GENERAL;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
32
Recensione:
Indirizzi per estratti:
Citazione:
D. Arnett, "OXYGEN-BURNING HYDRODYNAMICS .1. STEADY SHELL BURNING", The Astrophysical journal, 427(2), 1994, pp. 932-946

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 Ni-56 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.

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Documento generato il 27/11/20 alle ore 15:42:20