POST-SHOCK-REVIVAL EVOLUTION IN THE NEUTRINO-HEATING MECHANISM OF CORE-COLLAPSE SUPERNOVAE

Journal Article · Mon Jul 01 00:00:00 EDT 2013 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/771/1/27· OSTI ID:22140218

Yamamoto, Yu; Yamada, Shoichi ^[1]; Fujimoto, Shin-ichiro ^[2]; Nagakura, Hiroki ^[3]

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1. Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555 (Japan)
2. Kumamoto National College of Technology, 2659-2 Suya, Goshi, Kumamoto 861-1102 (Japan)
3. Yukawa Institute for Theoretical Physics, Kyoto University, Oiwake-cho, Kitashirakawa, Sakyo-ku, Kyoto 606-8502 (Japan)

We perform experimental simulations with spherical symmetry and axisymmetry to understand the post-shock-revival evolution of core-collapse supernovae. Assuming that the stalled shock wave is relaunched by neutrino heating and employing the so-called light bulb approximation, we induce shock revival by raising the neutrino luminosity up to the critical value, which is determined by dynamical simulations. A 15 M{sub Sun} progenitor model is employed. We incorporate nuclear network calculations with a consistent equation of state in the simulations to account for the energy release by nuclear reactions and their feedback to hydrodynamics. Varying the shock-relaunch time rather arbitrarily, we investigate the ensuing long-term evolutions systematically, paying particular attention to the explosion energy and nucleosynthetic yields as a function of relaunch time, or equivalently, the accretion rate at shock revival. We study in detail how the diagnostic explosion energy approaches the asymptotic value and which physical processes contribute in what proportions to the explosion energy. Furthermore, we study the dependence of physical processes on the relaunch time and the dimension of dynamics. We find that the contribution of nuclear reactions to the explosion energy is comparable to or greater than that of neutrino heating. In particular, recombinations are dominant over burnings in the contributions of nuclear reactions. Interestingly, one-dimensional (1D) models studied in this paper cannot produce the appropriate explosion energy and nickel mass simultaneously; nickels are overproduced. This problem is resolved in 2D models if the shock is relaunched at 300-400 ms after the bounce.

• OSTI ID: 22140218
• Journal Information: Astrophysical Journal, Vol. 771, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABUNDANCE
APPROXIMATIONS
ASYMPTOTIC SOLUTIONS
COMPARATIVE EVALUATIONS
EQUATIONS OF STATE
EXPLOSIONS
LIGHT BULBS
LUMINOSITY
MAGNETOHYDRODYNAMICS
NEUTRINOS
NICKEL
NUCLEAR REACTIONS
NUCLEOSYNTHESIS
ONE-DIMENSIONAL CALCULATIONS
SHOCK WAVES
SIMULATION
SPHERICAL CONFIGURATION
STAR EVOLUTION
SUPERNOVAE
SYMMETRY