Post-shock-revival evolution in the neutrino-heating mechanism of core-collapse supernovae

Yu Yamamoto, Shin Ichiro Fujimoto, Hiroki Nagakura, Shoichi Yamada

    Research output: Contribution to journalArticle

    15 Citations (Scopus)

    Abstract

    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 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.

    Original languageEnglish
    Article number27
    JournalAstrophysical Journal
    Volume771
    Issue number1
    DOIs
    Publication statusPublished - 2013 Jul 1

    Fingerprint

    supernovae
    neutrinos
    shock
    explosions
    explosion
    heating
    nuclear reactions
    energy
    nickel
    simulation
    symmetry
    shock wave
    equation of state
    recombination
    luminaires
    shock waves
    proportion
    equations of state
    hydrodynamics
    accretion

    Keywords

    • magnetohydrodynamics (MHD)
    • methods: numerical
    • nuclear reactions, nucleosynthesis, abundances
    • supernovae: general

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    Post-shock-revival evolution in the neutrino-heating mechanism of core-collapse supernovae. / Yamamoto, Yu; Fujimoto, Shin Ichiro; Nagakura, Hiroki; Yamada, Shoichi.

    In: Astrophysical Journal, Vol. 771, No. 1, 27, 01.07.2013.

    Research output: Contribution to journalArticle

    Yamamoto, Yu ; Fujimoto, Shin Ichiro ; Nagakura, Hiroki ; Yamada, Shoichi. / Post-shock-revival evolution in the neutrino-heating mechanism of core-collapse supernovae. In: Astrophysical Journal. 2013 ; Vol. 771, No. 1.
    @article{90df915fa6a54bc496fb69cf732f6430,
    title = "Post-shock-revival evolution in the neutrino-heating mechanism of core-collapse supernovae",
    abstract = "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⊙ 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.",
    keywords = "magnetohydrodynamics (MHD), methods: numerical, nuclear reactions, nucleosynthesis, abundances, supernovae: general",
    author = "Yu Yamamoto and Fujimoto, {Shin Ichiro} and Hiroki Nagakura and Shoichi Yamada",
    year = "2013",
    month = "7",
    day = "1",
    doi = "10.1088/0004-637X/771/1/27",
    language = "English",
    volume = "771",
    journal = "Astrophysical Journal",
    issn = "0004-637X",
    publisher = "IOP Publishing Ltd.",
    number = "1",

    }

    TY - JOUR

    T1 - Post-shock-revival evolution in the neutrino-heating mechanism of core-collapse supernovae

    AU - Yamamoto, Yu

    AU - Fujimoto, Shin Ichiro

    AU - Nagakura, Hiroki

    AU - Yamada, Shoichi

    PY - 2013/7/1

    Y1 - 2013/7/1

    N2 - 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⊙ 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.

    AB - 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⊙ 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.

    KW - magnetohydrodynamics (MHD)

    KW - methods: numerical

    KW - nuclear reactions, nucleosynthesis, abundances

    KW - supernovae: general

    UR - http://www.scopus.com/inward/record.url?scp=84879357542&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84879357542&partnerID=8YFLogxK

    U2 - 10.1088/0004-637X/771/1/27

    DO - 10.1088/0004-637X/771/1/27

    M3 - Article

    AN - SCOPUS:84879357542

    VL - 771

    JO - Astrophysical Journal

    JF - Astrophysical Journal

    SN - 0004-637X

    IS - 1

    M1 - 27

    ER -