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Title: The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M stars

Abstract

We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M 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 ≡ 1051 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 BS–1, respectively, for the 12, 15, 20, and 25 M 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 modelmore » in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. In conclusion, we compare our results for the explosion energies and ejected 56Ni masses against some observational standards despite the large error bars in both models and observations.« less

Authors:
 [1];  [2];  [2];  [2];  [3];  [4];  [4];  [5];  [3];  [6];  [7];  [4]
  1. Florida Atlantic Univ., Boca Raton, FL (United States)
  2. Univ. of Tennessee, Knoxville, TN (United States); Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
  3. Univ. of Tennessee, Knoxville, TN (United States)
  4. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States); Univ. of Tennessee, Knoxville, TN (United States)
  5. North Carolina State Univ., Raleigh, NC (United States)
  6. Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States)
  7. National Science Foundation, Arlington, VA (United States)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1238729
Grant/Contract Number:  
AC05-00OR22725l; AC02- 05CH11231; TGMCA08X010; OCI-0749248; OCI- 0749204; OCI-0749242
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 818; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Massive supernovae; stars evolution; neutrinos

Citation Formats

Bruenn, Stephen W., Lentz, Eric J., Hix, William Raphael, Mezzacappa, Anthony, Harris, James Austin, Messer, O. E. Bronson, Endeve, Eirik, Blondin, John M., Chertkow, Merek Austin, Lingerfelt, Eric J., Marronetti, Pedro, and Yakunin, Konstantin N. The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars. United States: N. p., 2016. Web. doi:10.3847/0004-637X/818/2/123.
Bruenn, Stephen W., Lentz, Eric J., Hix, William Raphael, Mezzacappa, Anthony, Harris, James Austin, Messer, O. E. Bronson, Endeve, Eirik, Blondin, John M., Chertkow, Merek Austin, Lingerfelt, Eric J., Marronetti, Pedro, & Yakunin, Konstantin N. The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars. United States. doi:10.3847/0004-637X/818/2/123.
Bruenn, Stephen W., Lentz, Eric J., Hix, William Raphael, Mezzacappa, Anthony, Harris, James Austin, Messer, O. E. Bronson, Endeve, Eirik, Blondin, John M., Chertkow, Merek Austin, Lingerfelt, Eric J., Marronetti, Pedro, and Yakunin, Konstantin N. Tue . "The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars". United States. doi:10.3847/0004-637X/818/2/123. https://www.osti.gov/servlets/purl/1238729.
@article{osti_1238729,
title = {The development of explosions in axisymmetric ab initio core-collapse supernova simulations of 12–25 M⊙ stars},
author = {Bruenn, Stephen W. and Lentz, Eric J. and Hix, William Raphael and Mezzacappa, Anthony and Harris, James Austin and Messer, O. E. Bronson and Endeve, Eirik and Blondin, John M. and Chertkow, Merek Austin and Lingerfelt, Eric J. and Marronetti, Pedro and Yakunin, Konstantin N.},
abstractNote = {We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25 M⊙ 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 ≡ 1051 erg) and increasing at 0.03, 0.15, 0.19, and 0.52 BS–1, respectively, for the 12, 15, 20, and 25 M⊙ 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⊙ model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. In conclusion, we compare our results for the explosion energies and ejected 56Ni masses against some observational standards despite the large error bars in both models and observations.},
doi = {10.3847/0004-637X/818/2/123},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 818,
place = {United States},
year = {2016},
month = {2}
}

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