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We propose that a significant fraction of the ultracompact HII regions foundin massive star-forming clouds are the result of the interaction of the windand ionizing radiation from a young massive star with the clumpy molecularcloud gas in its neighbourhood. Distributed mass loading in the flow allows thecompact nebulae to be long-lived. In this paper, we discuss a particularlysimple case, in which the flow in the HII region is everywhere supersonic. Theline profiles predicted for this model are highly characteristic, for the caseof uniform mass loading. We discuss briefly other observational diagnostics ofthese models.

Clumpy ultracompact H II regions – I. Fully supersonic wind-blown models