Anisotropies in the Neutrino Fluxes and Heating Profiles in Two-dimensional, Time-dependent, Multigroup Radiation Hydrodynamics Simulations of Rotating Core-Collapse Supernovae
Anisotropies in the Neutrino Fluxes and Heating Profiles in Two-dimensional, Time-dependent, Multigroup Radiation Hydrodynamics Simulations of Rotating Core-Collapse Supernovae
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旋转核心塌陷超新星的二维、时间相关、多群辐射流体动力学模拟中中微子通量和加热剖面的各向异性
DOI：
10.1086/429816
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发表时间：
2004
期刊：
影响因子：
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通讯作者：
M. Jarrah
中科院分区：
文献类型：
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作者：
R. Walder;Adam Burrows;Christian D. Ott;Eli Livne;I. Lichtenstadt;M. Jarrah
使用二维的，多群的，通量有限的扩散版本的代码VULCAN/2D，其中还包括旋转，我们已经计算了崩溃，反弹，冲击波的形成，和早期postbounce演化阶段的核心坍缩超新星的各种初始旋转速率。这是在超新星理论中使用全多维工具进行的第一系列此类多群计算。我们发现，虽然旋转产生极赤道角各向异性的中微子辐射场，不对称的幅度是不是像以前估计的那么大。中微子退偶表面的有限宽度和τ = 2/3表面上方的显着发射率缓和了角对比度。此外，我们发现辐射场总是比物质分布更具有球对称性，其羽流和对流涡旋。一点上的辐射场是来自不同贡献方向的许多源的积分。因此，它的分布比物质的分布平滑得多，并且在高空间频率下具有非常小的功率。给出了中微子场的角各向异性与中微子种类、中微子能量和初始转动速率的关系。只有对于我们最快速旋转的模型，我们才开始看到质的不同的流体动力学，但对于较低的速率与文献中推导出的塌陷前旋转轮廓一致的各向异性，虽然有趣，但是适度的。这并不意味着旋转在超新星动力学中不起关键作用。由于向心效应而导致的有效重力的减少可能是相当重要的。相反，这意味着，当一个真实的映射之间的初始和最终的旋转配置文件和二维多群辐射流体力学纳入崩溃模拟，辐射场的各向异性可能只是一个次要的，而不是一个关键的因素，在超新星的机制。
Using the two-dimensional, multigroup, flux-limited diffusion version of the code VULCAN/2D, which also incorporates rotation, we have calculated the collapse, bounce, shock formation, and early postbounce evolutionary phases of a core-collapse supernova for a variety of initial rotation rates. This is the first series of such multigroup calculations undertaken in supernova theory with fully multidimensional tools. We find that although rotation generates pole-to-equator angular anisotropies in the neutrino radiation fields, the magnitude of the asymmetries is not as large as previously estimated. The finite width of the neutrino decoupling surfaces and the significant emissivity above the τ = 2/3 surface moderate the angular contrast. Moreover, we find that the radiation field is always more spherically symmetric than the matter distribution, with its plumes and convective eddies. The radiation field at a point is an integral over many sources from the different contributing directions. As such, its distribution is much smoother than that of the matter and has very little power at high spatial frequencies. We present the dependence of the angular anisotropy of the neutrino fields on neutrino species, neutrino energy, and initial rotation rate. Only for our most rapidly rotating model do we start to see qualitatively different hydrodynamics, but for the lower rates consistent with the precollapse rotational profiles derived in the literature the anisotropies, although interesting, are modest. This does not mean that rotation does not play a key role in supernova dynamics. The decrease in the effective gravity due to the centripetal effect can be quite important. Rather, it means that when a realistic mapping between initial and final rotational profiles and two-dimensional multigroup radiation hydrodynamics are incorporated into collapse simulations, the anisotropy of the radiation fields may be only a secondary, not a pivotal, factor in the supernova mechanism.
巴塞尔大学（英国）
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长长中微子辐射在核心塌陷超新星中的重要性：SN1987A 长长几何形状的原因？
DOI：
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发表时间：
2004
期刊：
Pub. Astron. Soc. Japan 56
影响因子：
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作者：
H. Madokoro;T. Shimizu;Y. Motizuki
通讯作者：
Y. Motizuki