分子云中的超新星激波：分子氢的速度分布
Supernova Shocks in Molecular Clouds: Velocity Distribution of Molecular Hydrogen
摘要：
来自大质量恒星核心坍缩的超新星将冲击波驱动到恒星形成的分子云中。这种冲击会影响分子云未来的恒星形成，而快速移动的致密气体和压缩的磁场与增强的宇宙射线有关。本文介绍了利用Paris-Durham激波模型的新的理论模型，以及利用平流层红外天文台（SOFIA）对超新星遗迹IC 443分子激波H $_2$ S（5）纯旋转线的新观测。我们生成MHD模型的非稳态冲击驱动的压力的IC 443爆炸波到气体的密度$10^3$到$10^5$厘米$^{-3}$。我们提出了第一个详细的推导的速度分布的形状，从H $_2$线的发射后，这样的冲击，考虑到冲击年龄，震前密度，和磁场。对于震前密度$10^3$ - $10^5$ cm $^{-3}$，预测的H $_2$线的线中心位移和线宽度分别为20-2和30-4 km/s。先验模型进行了比较所观察到的线的轮廓，表明，团块C和G可以解释为冲击气体密度为10 $^3$到$2\times 10^4$厘米$^{-3}$和强磁场。对于团簇B2（靠近团簇B的较暗区域），H $_2$谱需要J型激波进入中等密度（约100 cm $^{-3}$），气体从其预激波位置加速到100 km/s。团块B1需要一个磁主导的C型激波（如团块C和G）和一个J型激波（如团块B1）来解释观测到的最高速度。产生高速分子的J型激波可能是磁场几乎平行于激波速度的位置，这使得C型激波（离子和中性粒子分离）不可能形成。
英文摘要：
Supernovae from core-collapse of massive stars drive shocks into the molecular clouds from which the stars formed. Such shocks affect future star formation from the molecular clouds, and the fast-moving, dense gas with compressed magnetic fields is associated with enhanced cosmic rays. This paper presents new theoretical modeling, using the Paris-Durham shock model, and new observations, using the Stratospheric Observatory for Infrared Astronomy (SOFIA), of the H$_2$ S(5) pure rotational line from molecular shocks in the supernova remnant IC443. We generate MHD models for non-steady-state shocks driven by the pressure of the IC443 blast wave into gas of densities $10^3$ to $10^5$ cm$^{-3}$. We present the first detailed derivation of the shape of the velocity profile for emission from H$_2$ lines behind such shocks, taking into account the shock age, preshock density, and magnetic field. For preshock densities $10^3$-$10^5$ cm$^{-3}$, the the predicted shifts of line centers, and the line widths, of the H$_2$ lines range from 20-2, and 30-4 km/s, respectively. The a priori models are compared to the observed line profiles, showing that clumps C and G can be explained by shocks into gas with density 10$^3$ to $2\times 10^4$ cm$^{-3}$ and strong magnetic fields. For clump B2 (a fainter region near clump B), the H$_2$ spectrum requires a J-type shock into moderate density (~100 cm$^{-3}$) with the gas accelerated to 100 km/s from its pre-shock location. Clump B1 requires both a magnetic-dominated C-type shock (like for clumps C and G) and a J-type shock (like for clump B1) to explain the highest observed velocities. The J-type shocks that produce high-velocity molecules may be locations where the magnetic field is nearly parallel to the shock velocity, which makes it impossible for a C-type shock (with ions and neutrals separated) to form.
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