Abstract
There has been considerable uncertainty in the nature of the regions from which carbon and narrow hydrogen lines have been observed. Specifically there are two different models. In model I the lines originate in low-density Hi regions that are basically atomic, and stimulated emission enhances the line intensity by an order of magnitude. In model II the lines originate in the outer layers of very dense molecular regions and are due primarily to spontaneous emission. The first model is generally accepted and used by the astronomical community. However, we believe that the second is correct.
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