NEUTRINO-DRIVEN TURBULENT CONVECTION and STANDING ACCRETION SHOCK INSTABILITY in THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE

Ernazar Abdikamalov, Christian D. Ott, David Radice, Luke F. Roberts, Roland Haas, Christian Reisswig, Philipp Mösta, Hannah Klion, Erik Schnetter

    Research output: Contribution to journalArticle

    42 Citations (Scopus)

    Abstract

    We conduct a series of numerical experiments into the nature of three-dimensional (3D) hydrodynamics in the postbounce stalled-shock phase of core-collapse supernovae using 3D general-relativistic hydrodynamic simulations of a 27 Mo progenitor star with a neutrino leakage/heating scheme. We vary the strength of neutrino heating and find three cases of 3D dynamics: (1) neutrino-driven convection, (2) initially neutrino-driven convection and subsequent development of the standing accretion shock instability (SASI), and (3) SASI-dominated evolution. This confirms previous 3D results of Hanke et al. and Couch & Connor. We carry out simulations with resolutions differing by up to a factor of ∼4 and demonstrate that low resolution is artificially favorable for explosion in the 3D convection-dominated case since it decreases the efficiency of energy transport to small scales. Low resolution results in higher radial convective fluxes of energy and enthalpy, more fully buoyant mass, and stronger neutrino heating. In the SASI-dominated case, lower resolution damps SASI oscillations. In the convection-dominated case, a quasi-stationary angular kinetic energy spectrum E(ℓ) develops in the heating layer. Like other 3D studies, we find E(ℓ) ∝ℓ-1 in the "inertial range," while theory and local simulations argue for E(ℓ) ∝ ℓ-5/3. We argue that current 3D simulations do not resolve the inertial range of turbulence and are affected by numerical viscosity up to the energy-containing scale, creating a "bottleneck" that prevents an efficient turbulent cascade.

    Original languageEnglish
    Article number70
    JournalAstrophysical Journal
    Volume808
    Issue number1
    DOIs
    Publication statusPublished - Jul 20 2015

    Fingerprint

    supernovae
    convection
    neutrinos
    shock
    accretion
    heating
    simulation
    hydrodynamics
    energy
    couches
    enthalpy
    kinetic energy
    leakage
    explosion
    viscosity
    turbulence
    oscillation
    explosions
    cascades
    energy spectra

    Keywords

    • hydrodynamics
    • neutrinos
    • supernovae: general

    ASJC Scopus subject areas

    • Nuclear and High Energy Physics

    Cite this

    NEUTRINO-DRIVEN TURBULENT CONVECTION and STANDING ACCRETION SHOCK INSTABILITY in THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE. / Abdikamalov, Ernazar; Ott, Christian D.; Radice, David; Roberts, Luke F.; Haas, Roland; Reisswig, Christian; Mösta, Philipp; Klion, Hannah; Schnetter, Erik.

    In: Astrophysical Journal, Vol. 808, No. 1, 70, 20.07.2015.

    Research output: Contribution to journalArticle

    Abdikamalov, Ernazar ; Ott, Christian D. ; Radice, David ; Roberts, Luke F. ; Haas, Roland ; Reisswig, Christian ; Mösta, Philipp ; Klion, Hannah ; Schnetter, Erik. / NEUTRINO-DRIVEN TURBULENT CONVECTION and STANDING ACCRETION SHOCK INSTABILITY in THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE. In: Astrophysical Journal. 2015 ; Vol. 808, No. 1.
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    AU - Ott, Christian D.

    AU - Radice, David

    AU - Roberts, Luke F.

    AU - Haas, Roland

    AU - Reisswig, Christian

    AU - Mösta, Philipp

    AU - Klion, Hannah

    AU - Schnetter, Erik

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    AB - We conduct a series of numerical experiments into the nature of three-dimensional (3D) hydrodynamics in the postbounce stalled-shock phase of core-collapse supernovae using 3D general-relativistic hydrodynamic simulations of a 27 Mo progenitor star with a neutrino leakage/heating scheme. We vary the strength of neutrino heating and find three cases of 3D dynamics: (1) neutrino-driven convection, (2) initially neutrino-driven convection and subsequent development of the standing accretion shock instability (SASI), and (3) SASI-dominated evolution. This confirms previous 3D results of Hanke et al. and Couch & Connor. We carry out simulations with resolutions differing by up to a factor of ∼4 and demonstrate that low resolution is artificially favorable for explosion in the 3D convection-dominated case since it decreases the efficiency of energy transport to small scales. Low resolution results in higher radial convective fluxes of energy and enthalpy, more fully buoyant mass, and stronger neutrino heating. In the SASI-dominated case, lower resolution damps SASI oscillations. In the convection-dominated case, a quasi-stationary angular kinetic energy spectrum E(ℓ) develops in the heating layer. Like other 3D studies, we find E(ℓ) ∝ℓ-1 in the "inertial range," while theory and local simulations argue for E(ℓ) ∝ ℓ-5/3. We argue that current 3D simulations do not resolve the inertial range of turbulence and are affected by numerical viscosity up to the energy-containing scale, creating a "bottleneck" that prevents an efficient turbulent cascade.

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