原始组分激波后冷却气体中H-$_2$和H-$_2^+$的态-态振动动力学
State-to-state vibrational kinetics of H$_2$ and H$_2^+$ in a post-shock cooling gas with primordial composition
摘要：
具有原始化学成分的冲击气体的辐射冷却是与第一批恒星和结构的形成有关的重要过程，也发生在高速云碰撞和超新星爆炸中。在需要考虑的不同过程中，分子氢的形成动力学和冷却是最重要的，因为它们提供了将气体温度降低到远低于$\sim$ 10 $^4$ ~K的值的唯一方法。在以前的工作中，H $_2$和它的阳离子的内能结构已经在低密度的振转基态近似下处理，或者试图用任意的$v>0$ H $_2$能级来描述动力学，该能级被认为是激发振动流形的代表。在这项研究中，我们计算的振动分辨动力学的时间依赖性的化学和热演化的后冲击气体在介质中的原始组成。计算的非平衡分布被用来评估对气体的冷却功能和冷却时间的影响。最后，我们讨论了结果对不同初始激波速度和红移的依赖性。
英文摘要：
The radiative cooling of shocked gas with primordial chemical composition is an important process relevant to the formation of the first stars and structures, as well as taking place also in high velocity cloud collisions and supernovae explosions. Among the different processes that need to be considered, the formation kinetics and cooling of molecular hydrogen are of prime interest, since they provide the only way to lower the gas temperature to values well below $\sim$10$^4$~K. In previous works, the internal energy level structure of H$_2$ and its cation has been treated in the approximation of rovibrational ground state at low densities, or trying to describe the dynamics using some arbitrary $v>0$ H$_2$ level that is considered representative of the excited vibrational manifold. In this study, we compute the vibrationally resolved kinetics for the time-dependent chemical and thermal evolution of the post-shock gas in a medium of primordial composition. The calculated non-equilibrium distributions are used to evaluate effects on the cooling function of the gas and on the cooling time. Finally, we discuss the dependence of the results to different initial values of the shock velocity and redshift.
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。
