Low Mach Number Modeling of Type Ia supernovae. IV. White Dwarf Convection [electronic resource]
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 tr...
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| Format: | Electronic eBook |
| Language: | English |
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Oak Ridge, Tenn. : Oak Ridge, Tenn. :
Oak Ridge National Laboratory ; Distributed by the Office of Scientific and Technical Information, U.S. Department of Energy,
2009.
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| Subjects: |
MARC
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| 245 | 0 | 0 | |a Low Mach Number Modeling of Type Ia supernovae. IV. White Dwarf Convection |h [electronic resource] |
| 260 | |a Oak Ridge, Tenn. : |b Oak Ridge National Laboratory ; |a Oak Ridge, Tenn. : |b Distributed by the Office of Scientific and Technical Information, U.S. Department of Energy, |c 2009. | ||
| 300 | |a Size: p. 196-210 : |b digital, PDF file. | ||
| 336 | |a text |b txt |2 rdacontent. | ||
| 337 | |a computer |b c |2 rdamedia. | ||
| 338 | |a online resource |b cr |2 rdacarrier. | ||
| 500 | |a Published through Scitech Connect. | ||
| 500 | |a 09/21/2009. | ||
| 500 | |a "Journal ID: ISSN 0004-637X" | ||
| 500 | |a Zingale, M. ; Almgren, A. S. ; Bell, J. B. ; Nonaka, A. ; Woosley, S. E. ; | ||
| 500 | |a USDOE Office of Science (SC) | ||
| 520 | 3 | |a 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. To conclude, we evolve several calculations to the point of ignition and discuss the range of ignition radii. | |
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| 650 | 7 | |a 79 astronomy and astrophysics |2 local. | |
| 650 | 7 | |a Astronomy & astrophysics |2 local. | |
| 650 | 7 | |a Convection |2 local. | |
| 650 | 7 | |a Hydrodynamics |2 local. | |
| 650 | 7 | |a Nuclear reactions |2 local. | |
| 650 | 7 | |a Nucleosynthesis |2 local. | |
| 650 | 7 | |a Abundances |2 local. | |
| 650 | 7 | |a Supernovae |2 local. | |
| 650 | 7 | |a White dwarfs |2 local. | |
| 710 | 2 | |a Oak Ridge National Laboratory. |4 res |4 spn. | |
| 710 | 1 | |a United States. |b Department of Energy. |b Office of Scientific and Technical Information |4 dst. | |
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