Shock evolution in non-radiative supernova remnants
Shock evolution in non-radiative supernova remnants
复制标题
非辐射超新星遗迹中的激波演化
DOI：
10.1093/mnras/stw2978
复制
发表时间：
2016
影响因子：
4.8
通讯作者：
R. Chevalier
中科院分区：
文献类型：
--
作者：
Xiaping Tang;R. Chevalier
本文提出了一种新的解析方法来获得描述非辐射超新星遗迹（SNRs）中激波演化的近似解。我们着重研究了前向激波和接触不连续性，而对反向激波的应用只作了简要的讨论。研究了具有等密度分布的星际介质和具有风密度分布的星周介质中SNR的球形激波演化。我们将新的解析解与数值模拟进行了比较，发现实现了百分之几的准确性。对于前向激波的演化，我们还将我们的新解与以前的分析模型进行了比较。在均匀的环境介质中，我们的分析近似的精度与Truelove&McKee（1999）相当。在风密度分布介质中，我们的解决方案比Micelotta等人（2016）更好，特别是当喷出物包络具有陡峭的密度分布时。新的解决方案是显着简化相比，以前的分析模型，因为它只依赖于其演变过程中的残留物的渐近行为。
We present a new analytical approach to derive approximate solutions describing the shock evolution in non-radiative supernova remnants (SNRs). We focus on the study of the forward shock and contact discontinuity while application to the reverse shock is only discussed briefly. The spherical shock evolution of a SNR in both the interstellar medium with a constant density profile and a circumstellar medium with a wind density profile is investigated. We compared our new analytical solution with numerical simulations and found that a few percent accuracy is achieved. For the evolution of the forward shock, we also compared our new solution to previous analytical models. In a uniform ambient medium, the accuracy of our analytical approximation is comparable to that in Truelove&McKee (1999). In a wind density profile medium, our solution performs better than that in Micelotta et al. (2016), especially when the ejecta envelope has a steep density profile. The new solution is significantly simplified compared to previous analytical models, as it only depends on the asymptotic behaviors of the remnant during its evolution.