The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M{sub ⊙} STARS

Bruenn, Stephen W.; Lentz, Eric J.; Mezzacappa, Anthony; Harris, J. Austin; Chertkow, Merek Austin; Yakunin, Konstantin N.; Hix, W. Raphael; Messer, O. E. Bronson; Endeve, Eirik; Lingerfelt, Eric J.; Blondin, John M.; Marronetti, Pedro

doi:10.3847/0004-637X/818/2/123

Title: The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M{sub ⊙} STARS

Journal Article · Sat Feb 20 00:00:00 EST 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/818/2/123· OSTI ID:22887018

Bruenn, Stephen W. ^[1]; Lentz, Eric J.; Mezzacappa, Anthony; Harris, J. Austin; Chertkow, Merek Austin; Yakunin, Konstantin N. ^[2]; Hix, W. Raphael ^[3]; Messer, O. E. Bronson ^[4]; Endeve, Eirik; Lingerfelt, Eric J. ^[5]; Blondin, John M. ^[6]; Marronetti, Pedro ^[7]

Department of Physics, Florida Atlantic University, 777 Glades Road, Boca Raton, FL 33431-0991 (United States)
Department of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996-1200 (United States)
Physics Division, Oak Ridge National Laboratory, P.O. Box 2008, Oak Ridge, TN 37831-6354 (United States)
National Center for Computational Sciences, Oak Ridge National Laboratory, P.O. Box 2008, Oak Ridge, TN 37831-6164 (United States)
Computer Science and Mathematics Division, Oak Ridge National Laboratory, P.O. Box 2008, Oak Ridge, TN 37831-6164 (United States)
Department of Physics, North Carolina State University, Raleigh, NC 27695-8202 (United States)
Physics Division, National Science Foundation, Arlington, VA 22207 (United States)

We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M{sub ⊙} zero-age main sequence progenitors. All of the simulations yield explosions and have been evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our Chimera code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B ≡ 10{sup 51} erg) and increasing at 0.03, 0.15, 0.19, and 0.52 B s{sup −1}, respectively, for the 12, 15, 20, and 25 M{sub ⊙} models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20 M{sub ⊙} model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected {sup 56}Ni masses against some observational standards despite the large error bars in both models and observations.

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OSTI ID:: 22887018

Journal Information:: Astrophysical Journal, Vol. 818, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Since 2009, the country of publication for this journal is the UK.; ISSN 0004-637X

Country of Publication:: United Kingdom

Language:: English

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Title: The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M{sub ⊙} STARS

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