SYSTEMATIC STUDIES of SHOCK REVIVAL and the SUBSEQUENT EVOLUTIONS in CORE-COLLAPSE SUPERNOVAE with PARAMETRIC PROGENITOR MODELS

Yu Yamamoto, Shoichi Yamada

    Research output: Contribution to journalArticle

    4 Citations (Scopus)

    Abstract

    We conducted one-dimensional and two-dimensional hydrodynamic simulations of post-shock revival evolutions in core-collapse supernovae, employing the simple neutrino light bulb approximation to produce explosions rather easily. In order to estimate the explosion energy, we took into proper account nuclear recombinations and fusions consistently with the equation of state for matter not in statistical equilibrium in general. The methodology is similar to our previous work, but is somehow improved. In this paper, we studied the influence of the progenitor structure on the dynamics systematically. In order to expedite our understanding of the systematics, we constructed six parametric progenitor models, which are different in masses of Fe iron core and Si+S layer, instead of employing realistic models provided by stellar evolution calculations, which are sometimes of stochastic nature as a function of stellar mass on the main sequence. We found that the explosion energy is tightly correlated with the mass accretion rate at shock revival irrespective of dimension and the progenitors with light iron cores but with rather high entropies, which have yet to be produced by realistic stellar evolution calculations, may reproduce the canonical values of explosion energy and nickel mass. The mass of the Si+S layer is also important in the mass accretion history after bounce, on the other hand; the higher mass accretion rates and resultant heavier cores tend to hamper strong explosions.

    Original languageEnglish
    Article number165
    JournalAstrophysical Journal
    Volume818
    Issue number2
    DOIs
    Publication statusPublished - 2016 Feb 20

    Fingerprint

    explosions
    explosion
    stellar evolution
    accretion
    shock
    iron
    energy
    stellar mass
    luminaires
    supernovae
    equation of state
    equations of state
    recombination
    neutrinos
    entropy
    fusion
    hydrodynamics
    histories
    nickel
    methodology

    Keywords

    • neutrinos
    • nuclear reactions, nucleosynthesis, abundances
    • stars: black holes
    • stars: massive
    • stars: neutron
    • supernovae: general

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

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    title = "SYSTEMATIC STUDIES of SHOCK REVIVAL and the SUBSEQUENT EVOLUTIONS in CORE-COLLAPSE SUPERNOVAE with PARAMETRIC PROGENITOR MODELS",
    abstract = "We conducted one-dimensional and two-dimensional hydrodynamic simulations of post-shock revival evolutions in core-collapse supernovae, employing the simple neutrino light bulb approximation to produce explosions rather easily. In order to estimate the explosion energy, we took into proper account nuclear recombinations and fusions consistently with the equation of state for matter not in statistical equilibrium in general. The methodology is similar to our previous work, but is somehow improved. In this paper, we studied the influence of the progenitor structure on the dynamics systematically. In order to expedite our understanding of the systematics, we constructed six parametric progenitor models, which are different in masses of Fe iron core and Si+S layer, instead of employing realistic models provided by stellar evolution calculations, which are sometimes of stochastic nature as a function of stellar mass on the main sequence. We found that the explosion energy is tightly correlated with the mass accretion rate at shock revival irrespective of dimension and the progenitors with light iron cores but with rather high entropies, which have yet to be produced by realistic stellar evolution calculations, may reproduce the canonical values of explosion energy and nickel mass. The mass of the Si+S layer is also important in the mass accretion history after bounce, on the other hand; the higher mass accretion rates and resultant heavier cores tend to hamper strong explosions.",
    keywords = "neutrinos, nuclear reactions, nucleosynthesis, abundances, stars: black holes, stars: massive, stars: neutron, supernovae: general",
    author = "Yu Yamamoto and Shoichi Yamada",
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    AU - Yamamoto, Yu

    AU - Yamada, Shoichi

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    AB - We conducted one-dimensional and two-dimensional hydrodynamic simulations of post-shock revival evolutions in core-collapse supernovae, employing the simple neutrino light bulb approximation to produce explosions rather easily. In order to estimate the explosion energy, we took into proper account nuclear recombinations and fusions consistently with the equation of state for matter not in statistical equilibrium in general. The methodology is similar to our previous work, but is somehow improved. In this paper, we studied the influence of the progenitor structure on the dynamics systematically. In order to expedite our understanding of the systematics, we constructed six parametric progenitor models, which are different in masses of Fe iron core and Si+S layer, instead of employing realistic models provided by stellar evolution calculations, which are sometimes of stochastic nature as a function of stellar mass on the main sequence. We found that the explosion energy is tightly correlated with the mass accretion rate at shock revival irrespective of dimension and the progenitors with light iron cores but with rather high entropies, which have yet to be produced by realistic stellar evolution calculations, may reproduce the canonical values of explosion energy and nickel mass. The mass of the Si+S layer is also important in the mass accretion history after bounce, on the other hand; the higher mass accretion rates and resultant heavier cores tend to hamper strong explosions.

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    KW - stars: massive

    KW - stars: neutron

    KW - supernovae: general

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