HST IMAGING OF THE WIND-BLOWN LOBE NGC 6165

WFC observations of the lobe NGC 6165 have resolved clumps that are be ing photoevaporated by the intense UV radiation from HD 148937, in add ition to the erosive effects of the strong stellar wind. The central o bject is a massive superluminous young star that is thought to be unde rgoing mass loss as it descends onto the main sequence. Analysis of se veral 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 10(17) cm . Calculations are made of the mass flow rates and of the gasdynamic p roperties of the flows, revealing that the clump is behaving much like a cometary structure. Ejection mechanisms from the central star are d iscussed with regard to the observed morphology of the nebula.