Revisiting impacts of nuclear burning for reviving weak shocks in neutrino-driven supernovae

Ko Nakamura, Tomoya Takiwaki, Kei Kotake, Nobuya Nishimura

    Research output: Contribution to journalArticle

    9 Citations (Scopus)

    Abstract

    We revisit potential impacts of nuclear burning on the onset of the neutrino-driven explosions of core-collapse supernovae. By changing the neutrino luminosity and its decay time to obtain parametric explosions in one- and two-dimensional (1D and 2D, respectively) models with or without a 13 isotope α network, we study how the inclusion of nuclear burning could affect the postbounce dynamics for 4 progenitor models; 3 for 15.0 M stars and 1 for an 11.2 M star. We find that the energy supply due to the nuclear burning of infalling material behind the shock can energize the shock expansion, especially for models that produce only marginal explosions in the absence of nuclear burning. These models are energized by nuclear energy deposition when the shock front passes through the silicon-rich layer and/or later as it touches the oxygen-rich layer. Depending on the neutrino luminosity and its decay time, the diagnostic energy of the explosion increases up to a few times 1050 erg for models with nuclear burning compared to the corresponding models without. We point out that these features are most remarkable for the Limongi-Chieffi progenitor in both 1D and 2D because the progenitor model possesses a massive oxygen layer, with an inner-edge radius that is smallest among the employed progenitors, which means that the shock can touch the rich fuel on a shorter timescale after bounce. The energy difference is generally smaller (0.1-0.2 × 1051 erg) in 2D than in 1D (at most 0.6 × 1051 erg). This is because neutrino-driven convection and the shock instability in 2D models enhance the neutrino heating efficiency, which makes the contribution of nuclear burning relatively smaller compared to 1D models. Considering uncertainties in progenitor models, our results indicate that nuclear burning should remain one of the important ingredients to foster the onset of neutrino-driven explosions.

    Original languageEnglish
    Article number91
    JournalAstrophysical Journal
    Volume782
    Issue number2
    DOIs
    Publication statusPublished - 2014 Feb 20

    Fingerprint

    supernovae
    neutrinos
    shock
    explosions
    explosion
    erg
    M stars
    touch
    luminosity
    oxygen
    shock fronts
    decay
    nuclear energy
    ingredients
    silicon
    energy
    convection
    isotopes
    inclusions
    isotope

    Keywords

    • Hydrodynamics
    • Neutrinos
    • Nuclear reactions: nucleosynthesis: abundances
    • Supernovae: general

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    Revisiting impacts of nuclear burning for reviving weak shocks in neutrino-driven supernovae. / Nakamura, Ko; Takiwaki, Tomoya; Kotake, Kei; Nishimura, Nobuya.

    In: Astrophysical Journal, Vol. 782, No. 2, 91, 20.02.2014.

    Research output: Contribution to journalArticle

    Nakamura, Ko ; Takiwaki, Tomoya ; Kotake, Kei ; Nishimura, Nobuya. / Revisiting impacts of nuclear burning for reviving weak shocks in neutrino-driven supernovae. In: Astrophysical Journal. 2014 ; Vol. 782, No. 2.
    @article{7d0bb25bac924870b15ca7788363a58a,
    title = "Revisiting impacts of nuclear burning for reviving weak shocks in neutrino-driven supernovae",
    abstract = "We revisit potential impacts of nuclear burning on the onset of the neutrino-driven explosions of core-collapse supernovae. By changing the neutrino luminosity and its decay time to obtain parametric explosions in one- and two-dimensional (1D and 2D, respectively) models with or without a 13 isotope α network, we study how the inclusion of nuclear burning could affect the postbounce dynamics for 4 progenitor models; 3 for 15.0 M stars and 1 for an 11.2 M star. We find that the energy supply due to the nuclear burning of infalling material behind the shock can energize the shock expansion, especially for models that produce only marginal explosions in the absence of nuclear burning. These models are energized by nuclear energy deposition when the shock front passes through the silicon-rich layer and/or later as it touches the oxygen-rich layer. Depending on the neutrino luminosity and its decay time, the diagnostic energy of the explosion increases up to a few times 1050 erg for models with nuclear burning compared to the corresponding models without. We point out that these features are most remarkable for the Limongi-Chieffi progenitor in both 1D and 2D because the progenitor model possesses a massive oxygen layer, with an inner-edge radius that is smallest among the employed progenitors, which means that the shock can touch the rich fuel on a shorter timescale after bounce. The energy difference is generally smaller (0.1-0.2 × 1051 erg) in 2D than in 1D (at most 0.6 × 1051 erg). This is because neutrino-driven convection and the shock instability in 2D models enhance the neutrino heating efficiency, which makes the contribution of nuclear burning relatively smaller compared to 1D models. Considering uncertainties in progenitor models, our results indicate that nuclear burning should remain one of the important ingredients to foster the onset of neutrino-driven explosions.",
    keywords = "Hydrodynamics, Neutrinos, Nuclear reactions: nucleosynthesis: abundances, Supernovae: general",
    author = "Ko Nakamura and Tomoya Takiwaki and Kei Kotake and Nobuya Nishimura",
    year = "2014",
    month = "2",
    day = "20",
    doi = "10.1088/0004-637X/782/2/91",
    language = "English",
    volume = "782",
    journal = "Astrophysical Journal",
    issn = "0004-637X",
    publisher = "IOP Publishing Ltd.",
    number = "2",

    }

    TY - JOUR

    T1 - Revisiting impacts of nuclear burning for reviving weak shocks in neutrino-driven supernovae

    AU - Nakamura, Ko

    AU - Takiwaki, Tomoya

    AU - Kotake, Kei

    AU - Nishimura, Nobuya

    PY - 2014/2/20

    Y1 - 2014/2/20

    N2 - We revisit potential impacts of nuclear burning on the onset of the neutrino-driven explosions of core-collapse supernovae. By changing the neutrino luminosity and its decay time to obtain parametric explosions in one- and two-dimensional (1D and 2D, respectively) models with or without a 13 isotope α network, we study how the inclusion of nuclear burning could affect the postbounce dynamics for 4 progenitor models; 3 for 15.0 M stars and 1 for an 11.2 M star. We find that the energy supply due to the nuclear burning of infalling material behind the shock can energize the shock expansion, especially for models that produce only marginal explosions in the absence of nuclear burning. These models are energized by nuclear energy deposition when the shock front passes through the silicon-rich layer and/or later as it touches the oxygen-rich layer. Depending on the neutrino luminosity and its decay time, the diagnostic energy of the explosion increases up to a few times 1050 erg for models with nuclear burning compared to the corresponding models without. We point out that these features are most remarkable for the Limongi-Chieffi progenitor in both 1D and 2D because the progenitor model possesses a massive oxygen layer, with an inner-edge radius that is smallest among the employed progenitors, which means that the shock can touch the rich fuel on a shorter timescale after bounce. The energy difference is generally smaller (0.1-0.2 × 1051 erg) in 2D than in 1D (at most 0.6 × 1051 erg). This is because neutrino-driven convection and the shock instability in 2D models enhance the neutrino heating efficiency, which makes the contribution of nuclear burning relatively smaller compared to 1D models. Considering uncertainties in progenitor models, our results indicate that nuclear burning should remain one of the important ingredients to foster the onset of neutrino-driven explosions.

    AB - We revisit potential impacts of nuclear burning on the onset of the neutrino-driven explosions of core-collapse supernovae. By changing the neutrino luminosity and its decay time to obtain parametric explosions in one- and two-dimensional (1D and 2D, respectively) models with or without a 13 isotope α network, we study how the inclusion of nuclear burning could affect the postbounce dynamics for 4 progenitor models; 3 for 15.0 M stars and 1 for an 11.2 M star. We find that the energy supply due to the nuclear burning of infalling material behind the shock can energize the shock expansion, especially for models that produce only marginal explosions in the absence of nuclear burning. These models are energized by nuclear energy deposition when the shock front passes through the silicon-rich layer and/or later as it touches the oxygen-rich layer. Depending on the neutrino luminosity and its decay time, the diagnostic energy of the explosion increases up to a few times 1050 erg for models with nuclear burning compared to the corresponding models without. We point out that these features are most remarkable for the Limongi-Chieffi progenitor in both 1D and 2D because the progenitor model possesses a massive oxygen layer, with an inner-edge radius that is smallest among the employed progenitors, which means that the shock can touch the rich fuel on a shorter timescale after bounce. The energy difference is generally smaller (0.1-0.2 × 1051 erg) in 2D than in 1D (at most 0.6 × 1051 erg). This is because neutrino-driven convection and the shock instability in 2D models enhance the neutrino heating efficiency, which makes the contribution of nuclear burning relatively smaller compared to 1D models. Considering uncertainties in progenitor models, our results indicate that nuclear burning should remain one of the important ingredients to foster the onset of neutrino-driven explosions.

    KW - Hydrodynamics

    KW - Neutrinos

    KW - Nuclear reactions: nucleosynthesis: abundances

    KW - Supernovae: general

    UR - http://www.scopus.com/inward/record.url?scp=84893584224&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84893584224&partnerID=8YFLogxK

    U2 - 10.1088/0004-637X/782/2/91

    DO - 10.1088/0004-637X/782/2/91

    M3 - Article

    AN - SCOPUS:84893584224

    VL - 782

    JO - Astrophysical Journal

    JF - Astrophysical Journal

    SN - 0004-637X

    IS - 2

    M1 - 91

    ER -