Shock–turbulence interaction in core-collapse supernovae
Shock–turbulence interaction in core-collapse supernovae
复制标题
核心塌陷超新星中的冲击-湍流相互作用
DOI：
10.1093/mnras/stw1604
复制
发表时间：
2016
影响因子：
4.8
通讯作者：
Caltech
中科院分区：
文献类型：
--
作者：
E. Abdikamalov;A. Zhaksylykov;D. Radice;S. B. N. University;Caltech
在大质量恒星生命的最后阶段，核壳燃烧伴随着强烈的湍流对流。由此产生的波动通过放大激波后区域的非径向流来帮助超新星爆炸。在这项工作中，我们使用线性微扰理论研究这种放大背后的物理机制。我们模拟的冲击波作为一个一维的平面不连续性，并考虑其与涡量和熵扰动的上游流的相互作用。我们发现，当扰动穿过激波时，它们的总湍流动能被放大了0.02倍，而湍流涡旋的平均线性尺寸减小了大约相同的因子。这些值对上游湍流参数和激波处的核解离效率不敏感。最后，我们讨论了我们的结果的超新星爆炸机制的含义。结果表明，上游扰动可以使中微子产生爆炸的临界亮度降低百分之几。
Nuclear shell burning in the final stages of the lives of massive stars is accompanied by strong turbulent convection. The resulting fluctuations aid supernova explosion by amplifying the non-radial flow in the post-shock region. In this work, we investigate the physical mechanism behind this amplification using a linear perturbation theory. We model the shock wave as a one-dimensional planar discontinuity and consider its interaction with vorticity and entropy perturbations in the upstream flow. We find that, as the perturbations cross the shock, their total turbulent kinetic energy is amplified by a factor of ∼2, while the average linear size of turbulent eddies decreases by about the same factor. These values are not sensitive to the parameters of the upstream turbulence and the nuclear dissociation efficiency at the shock. Finally, we discuss the implication of our results for the supernova explosion mechanism. We show that the upstream perturbations can decrease the critical neutrino luminosity for producing explosion by several per cent.
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