Abstract
WFC observations of the lobe NGC 6165 have resolved clumps that are being photoevaporated by the intense UV radiation from HD 148937, in addition to the erosive effects of the strong stellar wind. The central object is a massive superluminous young star that is thought to be undergoing mass loss as it descends onto the main sequence. Analysis of several of these clumps in more detail indicates the presence of strong shocks between the photoevaporated gas from the clump and the stellar wind itself. Typical sizes of the clumps appear to be around 1017cm. Calculations are made of the mass flow rates and of the gasdynamic properties of the flows, revealing that the clump is behaving much like a cometary structure. Ejection mechanisms from the central star are discussed with regard to the observed morphology of the nebula.
