NEUTRINO-DRIVEN TURBULENT CONVECTION AND STANDING ACCRETION SHOCK INSTABILITY IN THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE
NEUTRINO-DRIVEN TURBULENT CONVECTION AND STANDING ACCRETION SHOCK INSTABILITY IN THREE-DIMENSIONAL CORE-COLLAPSE SUPERNOVAE
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三维核心塌陷超新星中中微子驱动的湍流对流和静止吸积激波不稳定性
DOI：
10.1088/0004-637x/808/1/70
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
E. Schnetter
中科院分区：
文献类型：
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作者：
E. Abdikamalov;C. Ott;D. Radice;L. Roberts;R. Haas;C. Reisswig;P. Mösta;Hannah Klion;E. Schnetter
我们使用中微子泄漏/加热方案对 27 M⊙ 祖星进行 3D 广义相对论流体动力学模拟，对核心塌缩超新星弹跳后失速激波阶段的三维 (3D) 流体动力学性质进行了一系列数值实验。我们改变中微子加热的强度，发现了三种 3D 动力学情况：(1) 中微子驱动的对流，(2) 最初中微子驱动的对流和随后发展的常驻吸积激波不稳定性 (SASI)，以及 (3) SASI 主导的演化。这证实了 Hanke 等人之前的 3D 结果。以及沙发和康纳。我们以高达 4 倍的分辨率进行模拟，并证明低分辨率人为地有利于 3D 对流主导情况下的爆炸，因为它降低了小尺度能量传输的效率。低分辨率导致能量和热函的径向对流通量更高、浮力质量更充分以及中微子加热更强。在 SASI 主导的情况下，较低的分辨率会抑制 SASI 振荡。在对流主导的情况下，加热层中出现准稳态角动能谱 E(l)。与其他 3D 研究一样，我们发现 E(ℓ) ∝ℓ−1 在“惯性范围”内，而理论和局部模拟则认为 E(ℓ) ∝ ℓ−5/3。我们认为，当前的 3D 模拟无法解决湍流的惯性范围，并且会受到高达含能规模的数值粘度的影响，从而形成阻碍有效湍流级联的“瓶颈”。
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 M⊙ 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.
DOI：
10.1088/0004-637x/694/1/664
发表时间：
2007-08
期刊：
The Astrophysical Journal
影响因子：
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作者：
A. Marek;H. Janka
通讯作者：
A. Marek;H. Janka