Axisymmetric Ab Initio Core-Collapse Supernova Simulations of 12-25 M_sol Stars
| Autor: | W. Raphael Hix, Stephen W. Bruenn, Konstantin Yakunin, Eric J. Lentz, Anthony Mezzacappa, John M. Blondin, Eric J. Lingerfelt, Pedro Marronetti, O. E. Bronson Messer, Eirik Endeve |
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| Jazyk: | angličtina |
| Rok vydání: | 2012 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Physics Accretion (meteorology) 010308 nuclear & particles physics Ab initio FOS: Physical sciences Astronomy and Astrophysics Astrophysics Type II supernova Kinetic energy 7. Clean energy 01 natural sciences Shock (mechanics) Stars Supernova Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science 0103 physical sciences Neutrino Astrophysics - High Energy Astrophysical Phenomena 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) |
| Popis: | We present an overview of four ab initio axisymmetric core-collapse supernova simulations employing detailed spectral neutrino transport computed with our CHIMERA code and initiated from Woosley & Heger (2007) progenitors of mass 12, 15, 20, and 25 M_sol. All four models exhibit shock revival over \sim 200 ms (leading to the possibility of explosion), driven by neutrino energy deposition. Hydrodynamic instabilities that impart substantial asymmetries to the shock aid these revivals, with convection appearing first in the 12 M_sol model and the standing accretion shock instability (SASI) appearing first in the 25 M_sol model. Three of the models have developed pronounced prolate morphologies (the 20 M_sol model has remained approximately spherical). By 500 ms after bounce the mean shock radii in all four models exceed 3,000 km and the diagnostic explosion energies are 0.33, 0.66, 0.65, and 0.70 Bethe (B = $10^{51}$ ergs) for the 12, 15, 20, and 25 M_sol models, respectively, and are increasing. The three least massive of our models are already sufficiently energetic to completely unbind the envelopes of their progenitors (i.e., to explode), as evidenced by our best estimate of their explosion energies, which first become positive at 320, 380, and 440 ms after bounce. By 850 ms the 12 M_sol diagnostic explosion energy has saturated at 0.38 B, and our estimate for the final kinetic energy of the ejecta is \sim 0.3 B, which is comparable to observations for lower-mass progenitors. Accepted for publication in The Astrophysical Journal Letters |
| Databáze: | OpenAIRE |
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