W28与IC443激波中CO谱线轮廓的建模
Modeling CO Line Profiles in Shocks of W28 and IC44
AI总结：
本文结合Paris-Durham一维激波模型与LVG辐射转移框架，建模W28和IC443中慢速磁化C型激波的CO谱线轮廓，证明其可用更少谱线约束激波速度与激波前密度。
摘要：
由超新星遗迹（SNR）激波与分子云相互作用产生的分子发射，为研究可能触发恒星形成的弥散和压缩过程，以及理解超新星遗迹中的宇宙线增强提供了工具。在超新星遗迹—分子云相互作用中，磁流体动力学激波产生的纯转动CO发射是一种有效的激波示踪剂，尤其适用于进入分子云寒冷内部团块的慢速、连续激波。在本工作中，我们提出了一个新的理论辐射转移框架，利用Paris-Durham一维激波模型预测CO的谱线轮廓。我们针对密度约100,000 cm^-3的气体中、激波速度为35和50 km s^-1的慢速磁化C型激波所产生的CO发射，生成了谱线轮廓预测。用于再现CO谱线轮廓的数值框架采用大速度梯度（LVG）近似，并省略光厚平面平行板。借助该框架，我们对超新星遗迹W28和IC443中最高至J=16的多种CO光谱观测生成了预测；这些观测由SOFIA、IRAM-30m、APEX和KPNO获得。我们发现，CO谱线轮廓预测能够对激波速度和激波前密度提供约束，且这种约束独立于绝对谱线亮度，并比使用转动激发图的诊断方法需要更少的CO谱线。
英文摘要：
Molecular emission arising from the interactions of supernova remnant (SNR) shock waves and molecular clouds provide a tool for studying the dispersion and compression that might kick-start star formation as well as understanding cosmic ray enhancement in SNRs. Purely-rotational CO emission created by magneto-hydrodynamic shock in the SNR - molecular cloud interaction is an effective shock tracer, particularly for slow-moving, continuous shocks into cold inner clumps of the molecular cloud. In this work, we present a new theoretical radiative transfer framework for predicting the line profile of CO with the Paris-Durham 1D shock model. We generated line profile predictions for CO emission produced by slow, magnetized C-shocks into gas of density ~ 100,000 cm-3 with shock speeds of 35 and 50 km s-1. The numerical framework to reproduce the CO line profile utilizes the Large Velocity Gradient (LVG) approximation and the omission of optically-thick plane-parallel slabs. With this framework, we generated predictions for various CO spectroscopic observations up to J=16 in SNRs W28 and IC443, obtained with SOFIA, IRAM-30m, APEX, and KPNO. We found that CO line profile prediction offers constraints on the shock velocity and preshock density independent of the absolute line brightness and requiring fewer CO lines than diagnostics using an rotational excitation diagram.
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