Shock waves in the interstellar medium
Shock waves in the interstellar medium
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DOI：
10.1086/190562
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发表时间：
1979
影响因子：
8.7
通讯作者：
J. Raymond
中科院分区：
文献类型：
--
作者：
J. Raymond
本文给出了星际介质中平面平行稳态激波的光学和紫外发射线强度和离子柱密度的计算。考虑的冲击速度范围为50 km /s /sup -1/ <或=..nu../sub s/<或= 200km s/sup -1/，预震密度为1cm /sup -3/ <或=n/sub 0/<或= 300cm /sup -3/。发现预震气体的电离状态是一个重要的参数，并使用了几组元素丰度，对应于对颗粒的各种损耗量。这些结果与天鹅座环、船帆座超新星遗迹和赫比格-哈罗天体的观测结果进行了比较。
Calculations of the optical and UV emission-line intensities and column densities of ions observable in the optical and UV are presented for plane-parallel, steady-state shock waves in the interstellar medium. The range of shock velocities considered is 50 km s/sup -1/ < or =..nu../sub s/< or =200 km s/sup -1/, and preshock densities are 1 cm/sup -3/ < or =n/sub 0/< or =300 cm/sup -3/. The ionization state of the preshock gas is found to be an important parameter, and several sets of elemental abundances corresponding to various amounts of depletion onto grains are used. The results are compared with observations of the Cygnus Loop, the Vela supernova remnant, and Herbig-Haro objects.