Journal
ASTROPHYSICAL JOURNAL
Volume 734, Issue 1, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/734/1/37
Keywords
hydrodynamics; methods: numerical; shock waves; supernovae: general; turbulence
Categories
Funding
- DOE [DE-FC02-06ER41438]
- National Science Foundation [AST 0909129]
- NASA [NNX09AK36G]
- US Department of Energy, Office of Basic Energy Sciences, Division of Chemical Sciences, Geosciences and Biosciences
- US Department of Energy [DE-AC04-94AL85000, DE-AC02-05CH11231]
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The flame in a Type Ia supernova is a conglomerate structure that, depending on density, may involve separate regions of carbon, oxygen, and silicon burning, all propagating in a self-similar, subsonic front. The separation between these three burning regions increases as the density declines until eventually, below about 2 x 10(7) g cm(-3), only carbon burning remains active, the other two burning phases having frozen out on stellar scales. Between 2 and 3 x 10(7) g cm(-3), however, there remains an energetic oxygen-burning region that trails the carbon burning by an amount that is sensitive to the turbulence intensity. As the carbon flame makes a transition to the distributed regime (Karlovitz number greater than or similar to 10), the characteristic separation between the carbon-and oxygen-burning regions increases dramatically, from a fraction of a meter to many kilometers. The oxygen-rich mixture between the two flames is created at a nearly constant temperature, and turbulence helps to maintain islands of well-mixed isothermal fuel as the temperature increases. The delayed burning of these regions can be supersonic and could initiate a detonation.
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