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2D Simulations of Supernovae

Published online by Cambridge University Press:  12 April 2016

David Arnett
David Arnett*
Affiliation:
Steward Observatory, University of Arizona, Tucson, AZ 85721, USA

Abstract

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Several multidimensional computations of hydrodynamics related to supernovae have been completed, and are summarized here. More detail may be found in Arnett 1994a,b, Arnett & Livne 1994a,b, and Livne & Arnett 1993. The hydro code PROMETHEUS is based upon an implementation of the piecewise-parabolic method (PPM) of Colella & Woodward 1984, as described in Fryxell et al. 1991. A detailed comparison of PPM with other schemes is given in Woodward & Colella 1984. The method constructs the physics of the flow between grid points by a nonlinear solution of the equations of continuity of mass, momentum and energy (the Riemann problem) rather than the usual mathematical approach of a Taylor expansion about the grid points. This gives it better resolution per grid point, which is highly desirable for multidimensional problems. Although the effort required per grid point is greater, the number of such points is less (often much less) for a given level of accuracy. Because the computational load per grid point is greater, more realistic physics (reactions, radiation, gravity, etc.) may be added before affecting the runtime significantly. Thus PPM is well suited for multidimensional problems with significant physics beyond the bare hydrodynamics.

Type
Type la Supernovae
Information
International Astronomical Union Colloquium , Volume 145: Supernovae and Supernova Remnants , 1996 , pp. 91 - 98
Copyright
Copyright © Cambridge University Press 1996

References

Arnett, D. 1972a, Ap. J., 173, 393 Google Scholar
Arnett, D. 1972b, Ap. J., 176, 699 Google Scholar
Arnett, D. 1977, Ap. J., 218, 815 Google Scholar
Arnett, D. 1994a, Ap. J., 427, 932 Google Scholar
Arnett, D. 1994b, in preparation.Google Scholar
Arnett, D., Fryxell, B. A., & Müller, E., 1989, Ap. J. Lett, 341, L63 Google Scholar
Arnett, D. & Livne, E., 1994a Ap. J., 427, 315 Google Scholar
Arnett, D. & Livne, E., 1994b Ap. J., 427, 320 Google Scholar
Blondin, J. M., Stevens, I. R., & Kallman, T. R., 1991, Ap. J., 371, 684 Google Scholar
Cattaneo, F., Brummel, N. H., Toomre, J., Malagoli, A., & Hurlburt, N. E., 1991, Ap. J., 370, 282 Google Scholar
Colella, P. & Glaz, H. M., 1985, J. Comput. Phys., 59, 264 Google Scholar
Colella, P. & Woodward, P. R., 1984, J. Comput. Phys., 54, 174 Google Scholar
Fryxell, B. A., Müller, E. & Arnett, D., 1989, Numerical Methods in Astrophysics, ed. Paul R. Woodward, to have been published in Computational Techniques by Academic Press; preprint MPA 449, Max-Planck-Institut für Astrophysik, Garching Google Scholar
Fryxell, B. A., Müller, E. & Arnett, D., 1991, Ap. J., 367, 619 Google Scholar
Khokhlov, A. 1991, A. & Ap., 245, L25 Google Scholar
Livne, E., 1993, Ap. J. Lett, 406, L17 Google Scholar
Livne, E. and Arnett, D., 1993, Ap. J. Lett, 415, L107 Google Scholar
Müller, E., Fryxell, B. A., and Arnett, W. D., 1991, A. & Ap., 251, 505 Google Scholar
Nomoto, K., Sugimoto, D., and Neo, S. 1976, Astrophys. Space Sei., 39, 137 Google Scholar
Nomoto, K., Thielemann, F. K., & Yokoi, K. 1984, Ap. J.286, 644 Google Scholar
Timmes, X. and Woosley, S. E., 1992, Ap. J., 396, 649 Google Scholar
Woodward, P. R., & Colella, P. 1984, J. Comput. Phys., 54, 115 Google Scholar
Woosley, S. E., 1990, in Supernovae, ed. Petschek, A. G. (Dordrecht: Kluwer), 182.Google Scholar
Zeldovich, Ya. B. Barenblat, G. I., Librovich, V. B., & Mikhviladze, G. M., 1985, (New York: Consultants Bureau/Plenum).Google Scholar