Journal
ASTROPHYSICAL JOURNAL
Volume 785, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/785/1/61
Keywords
binaries: close; nuclear reactions, nucleosynthesis, abundances; shock waves; supernovae: general; white dwarfs
Categories
Funding
- National Science Foundation [PHY 11-25915, AST 11-09174]
- NASA through Einstein Postdoctoral Fellowship [PF-1120088]
- Chandra X-ray Center
- Smithsonian Astrophysical Observatory for NASA [NAS8-03060]
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1109174] Funding Source: National Science Foundation
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The progenitor channel responsible for the majority of Type Ia supernovae is still uncertain. One emergent scenario involves the detonation of a He-rich layer surrounding a C/O white dwarf, which sends a shock wave into the core. The quasi-spherical shock wave converges and strengthens at an off-center location, forming a second, C-burning, detonation that disrupts the whole star. In this paper, we examine this second detonation of the double detonation scenario using a combination of analytic and numeric techniques. We perform a spatially resolved study of the imploding shock wave and outgoing detonation and calculate the critical imploding shock strengths needed to achieve a core C detonation. We find that He detonations in recent two-dimensional simulations yield converging shock waves that are strong enough to ignite C detonations in high-mass C/O cores, with the caveat that a truly robust answer requires multi-dimensional detonation initiation calculations. We also find that convergence-driven detonations in low-mass C/O cores and in O/Ne cores are harder to achieve and are perhaps unrealized in standard binary evolution.
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