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Title:
Low Mach Number Modeling of Type IA Supernovae. IV. White Dwarf Convection
Authors:
Zingale, M.; Almgren, A. S.; Bell, J. B.; Nonaka, A.; Woosley, S. E.
Affiliation:
AA(Department of Physics & Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA ), AB(Center for Computational Sciences and Engineering, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA ), AC(Center for Computational Sciences and Engineering, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA ), AD(Center for Computational Sciences and Engineering, Lawrence Berkeley National Laboratory, Berkeley, CA 94720, USA ), AE(Department of Astronomy & Astrophysics, The University of California, Santa Cruz, Santa Cruz, CA 95064, USA)
Publication:
The Astrophysical Journal, Volume 704, Issue 1, pp. 196-210 (2009). (ApJ Homepage)
Publication Date:
10/2009
Origin:
IOP
ApJ Keywords:
convection, hydrodynamics, methods: numerical, nuclear reactions, nucleosynthesis, abundances, supernovae: general, white dwarfs
DOI:
10.1088/0004-637X/704/1/196
Bibliographic Code:
2009ApJ...704..196Z

Abstract

We present the first three-dimensional, full-star simulations of convection in a white dwarf preceding a Type Ia supernova, specifically the last few hours before ignition. For these long-time calculations, we use our low Mach number hydrodynamics code, MAESTRO, which we have further developed to treat spherical stars centered in a three-dimensional Cartesian geometry. The main change required is a procedure to map the one-dimensional radial base state to and from the Cartesian grid. Our models recover the dipole structure of the flow seen in previous calculations, but our long-time integration shows that the orientation of the dipole changes with time. Furthermore, we show the development of gravity waves in the outer, stable portion of the star. Finally, we evolve several calculations to the point of ignition and discuss the range of ignition radii.
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