年轻星系中超新星爆炸引发的恒星形成
Star Formation Triggered by Supernova Explosions in Young Galaxies
摘要：
本文用一维非平衡化学流体力学方法研究了早期宇宙中低金属丰度介质$Z/Z_{\odot} = 10^{-4}$ -$10^{-2}$中超新星遗迹的演化。一旦激波后层能够辐射冷却，激波后就会形成致密的壳层。如果这个壳层在引力作用下变得不稳定并碎裂成碎片，下一代恒星有望从这些碎片中形成。为了探索这种触发恒星形成的可能性，我们应用线性扰动分析的膨胀壳我们的结果和约束的参数范围的环境密度，爆炸能量，和金属丰度的外壳碎片发生。对于$10^{51}{\rm ergs} (10^{52}{\rm ergs})$的爆炸能量，当环境密度高于$\gtrsim 10^{2} {\rm cm^{-3}}$（分别为10 ${\rm cm^{-3}}$）时，发生壳层碎裂。在我们所考察的范围内，这个条件几乎不依赖于金属丰度。我们发现，触发的恒星形成模式只发生在大质量（$\gtrsim 10^{8}M_{\odot}$）晕。
英文摘要：
We study the evolution of supernova remnants in a low-metallicity medium $Z/Z_{\odot} = 10^{-4}$ -- $10^{-2}$ in the early universe, using one-dimensional hydrodynamics with non-equilibrium chemistry. Once a post-shock layer is able to cool radiatively, a dense shell forms behind the shock. If this shell becomes gravitationally unstable and fragments into pieces, next-generation stars are expected to form from these fragments. To explore the possibility of this triggered star formation, we apply a linear perturbation analysis of an expanding shell to our results and constrain the parameter range of ambient density, explosion energy, and metallicity where fragmentation of the shell occurs. For the explosion energy of $10^{51}{\rm ergs} (10^{52}{\rm ergs})$, the shell fragmentation occurs for ambient densities higher than $\gtrsim 10^{2} {\rm cm^{-3}}$ (10 ${\rm cm^{-3}}$, respectively). This condition depends little on the metallicity in the ranges we examined. We find that the mode of star formation triggered occurs only in massive ($\gtrsim 10^{8}M_{\odot}$) haloes.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
