THERMAL BALANCE IN DENSE MOLECULAR CLOUDS - RADIATIVE COOLING RATES AND EMISSION-LINE LUMINOSITIES

被引:244
作者
NEUFELD, DA
LEPP, S
MELNICK, GJ
机构
[1] UNIV NEVADA,DEPT PHYS,LAS VEGAS,NV 89154
[2] HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138
关键词
ISM; CLOUDS; MOLECULES; MOLECULAR PROCESSES; RADIATIVE TRANSFER; RADIO LINES;
D O I
10.1086/192211
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We consider the radiative cooling of fully shielded molecular astrophysical gas over a wide range of temperatures (10 K less than or equal to T less than or equal to 2500 K) and Ha densities (10(3) cm(-3) less than or equal to n(H-2) less than or equal to 10(10) cm(-3)). Our model for the radiative cooling of molecular gas includes a detailed treatment of the interstellar chemistry that determines the abundances of important coolant molecules, and a detailed treatment of the excitation of the species H-2, CO, H2O, HCl, O-2 C, O, and their isotopic variants where important. We present results for the total radiative cooling rate and for the cooling rate due to individual coolant species, as a function of the gas temperature, density, and optical depth. We have also computed the individual millimeter, submillimeter, and far-infrared line strengths that contribute to the total radiative cooling rate, and we have obtained example spectra for the submillimeter emission expected from molecular cloud cores. Many of the important cooling lines will be detectable using the Infrared Space Observatory and the Submillimeter Wave Astronomy Satellite.
引用
收藏
页码:132 / 147
页数:16
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