Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout
Three-dimensional simulations of core-collapse supernovae: from shock revival to shock breakout
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DOI：
10.1051/0004-6361/201425025
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发表时间：
2014-09
影响因子：
6.5
通讯作者：
A. Wongwathanarat;E. Mueller;H. J. M. Astrophysics;Riken
中科院分区：
文献类型：
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作者：
A. Wongwathanarat;E. Mueller;H. J. M. Astrophysics;Riken
我们提出了3D模拟的核心坍缩超新星从爆炸波启动的中微子驱动的机制，从恒星表面的冲击爆发，考虑两个15 Msun的红超巨星（RSG）和两个蓝超巨星（BSG）的15 Msun和20 Msun。我们表明，富含金属的喷出物在同源扩张仍然进行指纹的不对称性在爆炸开始时，但最终的金属分布是大规模的影响，详细的祖结构。扩展最快的金属指状物和团块与中微子加热物质的最大和上升最快的羽流相关，因为这些羽流在SN激波通过后最有效地在C+O/He和He/H组分-壳层界面处播种瑞利-泰勒（RT）不稳定性的增长。径向混合的程度、富金属喷出物的全球不对称性、RT诱导的初始羽流碎裂成较小尺度的指状物以及最大Ni和最小H速度不仅取决于初始非球面度和爆炸能量（这决定了激波和初始Ni速度），而且还取决于C+O核和He壳的密度分布和宽度以及He/H转变处的密度梯度，这导致不稳定的激波传播和反向激波的形成。这两个RSG爆炸保留了一个伟大的全球金属不对称性与显着的块状和子结构，深入渗透的镍手指到H-信封（最大速度为4000-5000公里/秒的爆炸能量约1.5倍）和有效的向内H-混合。虽然15 Msun BSG具有这些特性（最大Ni速度高达~3500 km/s），但20 Msun BSG由于反向激波减速和He/H界面处没有足够的时间进行强RT增长和碎裂，因此形成了更圆的几何形状，没有明显的金属指（最大Ni速度仅~2200 km/s）。
We present 3D simulations of core-collapse supernovae from blast-wave initiation by the neutrino-driven mechanism to shock breakout from the stellar surface, considering two 15 Msun red supergiants (RSG) and two blue supergiants (BSG) of 15 Msun and 20 Msun. We demonstrate that the metal-rich ejecta in homologous expansion still carry fingerprints of asymmetries at the beginning of the explosion, but the final metal distribution is massively affected by the detailed progenitor structure. The most extended and fastest metal fingers and clumps are correlated with the biggest and fastest-rising plumes of neutrino-heated matter, because these plumes most effectively seed the growth of Rayleigh-Taylor (RT) instabilities at the C+O/He and He/H composition-shell interfaces after the passage of the SN shock. The extent of radial mixing, global asymmetry of the metal-rich ejecta, RT-induced fragmentation of initial plumes to smaller-scale fingers, and maximal Ni and minimal H velocities do not only depend on the initial asphericity and explosion energy (which determine the shock and initial Ni velocities) but also on the density profiles and widths of C+O core and He shell and on the density gradient at the He/H transition, which lead to unsteady shock propagation and the formation of reverse shocks. Both RSG explosions retain a great global metal asymmetry with pronounced clumpiness and substructure, deep penetration of Ni fingers into the H-envelope (with maximum velocities of 4000-5000 km/s for an explosion energy around 1.5 bethe) and efficient inward H-mixing. While the 15 Msun BSG shares these properties (maximum Ni speeds up to ~3500 km/s), the 20 Msun BSG develops a much more roundish geometry without pronounced metal fingers (maximum Ni velocities only ~2200 km/s) because of reverse-shock deceleration and insufficient time for strong RT growth and fragmentation at the He/H interface.