Core-collapse supernova simulations in one and two dimensions: comparison of codes and approximations
Core-collapse supernova simulations in one and two dimensions: comparison of codes and approximations
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一维和二维核心塌缩超新星模拟：代码和近似值的比较
DOI：
10.1093/mnras/sty2578
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发表时间：
2018
影响因子：
4.8
通讯作者：
iTHEMS Riken
中科院分区：
文献类型：
--
作者：
O. Just;R. Bollig;H. Janka;M. Obergaulinger;R. Glas;Shigehiro Nagataki Abbl Riken;Saitama;Mpa Astrophysics;Garching;Tum;Univ. Valencia;iTHEMS Riken
我们提出了对流主导的 9 兆太阳和 20 兆太阳前体的球对称 (1D) 和轴对称 (2D) 超新星模拟，这些超新星通过站立吸积激波不稳定性 (SASI) 产生剧烈活动。我们详细比较了 Aenus-Alcar 代码（它使用带有 M1 闭包的完全多维两矩中微子传输）、该代码的逐射线加 (RbR+) 版本以及使用带有玻尔兹曼闭包的 RbR+ 两矩传输的 Prometheus-Vertex 代码。除了测试 RbR+ 近似中被忽略的非径向中微子通量分量的结果之外，我们还讨论了最近文献中应用或未应用的各种输运成分的影响，即简化的中微子对过程、中微子电子散射、速度相关项和引力红移项，以及中微子核散射的奇异性和多体校正。 Alcar 和 Vertex 在 1D 和 2D 方面表现出极好的一致性，尽管原中子星与 Alcar 的半径稍小但系统地较小（约 1 公里）且对流较强。如前所述，RbR+ 近似有利于爆炸，但在对流主导的 9 Msun 情况下，其严重程度远低于边缘爆炸的 20 Msun 模型，其中爆炸的开始时间也表现出较大的随机变化，并且 RbR+ 近似没有比简化对过程或奇异性和多体校正具有明显更强的支持效果。忽略中微子电子散射显然对爆炸有不利影响，而忽略速度和引力红移效应既可以促进也可以延迟爆炸。一维模拟中平流时间尺度与中微子加热时间尺度的比率是多维模拟中物理成分对爆炸影响的敏感指标。
We present spherically symmetric (1D) and axisymmetric (2D) supernova simulations for a convection-dominated 9 Msun and a 20 Msun progenitor that develops violent activity by the standing-accretion-shock instability (SASI). We compare in detail the Aenus-Alcar code, which uses fully multidimensional two-moment neutrino transport with an M1 closure, with a ray-by-ray-plus (RbR+) version of this code and with the Prometheus-Vertex code that employs RbR+ two-moment transport with a Boltzmann closure. Besides testing consequences of ignored non-radial neutrino-flux components in the RbR+ approximation, we also discuss the influence of various transport ingredients applied or not applied in recent literature, namely simplified neutrino-pair processes, neutrino-electron scattering, velocity-dependent and gravitational-redshift terms, and strangeness and many-body corrections for neutrino-nucleon scattering. Alcar and Vertex show excellent agreement in 1D and 2D despite a slightly but systematically smaller radius (~1km) and stronger convection of the proto-neutron star with Alcar. As found previously, the RbR+ approximation is conducive to explosions, but much less severely in the convection-dominated 9 Msun case than in the marginally exploding 20 Msun model, where the onset time of explosion also exhibits big stochastic variations, and the RbR+ approximation has no distinctly stronger supportive effect than simplified pair processes or strangeness and many-body corrections. Neglecting neutrino-electron scattering has clearly unfavorable effects for explosions, while ignoring velocity and gravitational-redshift effects can both promote or delay the explosion. The ratio of advection timescale to neutrino-heating timescale in 1D simulations is a sensitive indicator of the influence of physics ingredients on explosions also in multidimensional simulations.
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电子捕获和低质量铁核塌陷超新星：新的中微子辐射流体动力学模拟
DOI：
10.3847/1538-4357/aa92c5
发表时间：
2017
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Radice, David;Burrows, Adam;Vartanyan, David;Skinner, M. Aaron;Dolence, Joshua C.
通讯作者：
Dolence, Joshua C.
DOI：
10.1146/annurev-nucl-102115-044747
发表时间：
2016-02
影响因子：
12.4
作者：
H. Janka;T. Melson;A. S. M. Astrophysics;Garching;Physik Dept.;Tum
通讯作者：
H. Janka;T. Melson;A. S. M. Astrophysics;Garching;Physik Dept.;Tum
核心塌缩超新星机制的关键物理依赖性
影响因子：
10.3
作者：
Burrows, A.;Vartanyan, D.;Dolence, J. C.;Skinner, M. A.;Radice, D.
通讯作者：
Radice, D.
影响因子：
4.8
作者：
Just, O.;Bauswein, A.;Janka, H-T
通讯作者：
Janka, H-T