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The observed parameters of the young superstar cluster M82-A1 and itsassociated compact HII region are here shown to indicate a low heatingefficiency or immediate loss, through radiative cooling, of a large fraction ofthe energy inserted by stellar winds and supernovae during the early evolutionof the cluster. This implies a bimodal hydrodynamic solution which leads to areduced mass deposition rate into the ISM, with a much reduced outflowvelocity. Furthermore, to match the observed parameters of the HII regionassociated to M82-A1, the resultant star cluster wind is here shown to ought tobe confined by a high pressure interstellar medium. The cluster windparameters, as well as the location of the reverse shock, its cooling lengthand the radius of the standing outer HII region are derived analytically. Allof these properties are then confirmed with a semi-analytical integration ofthe flow equations, which provides us also with the run of the hydrodynamicvariables as a function of radius. The impact of the results is discussed andextended to other massive and young superstar clusters surrounded by a compactHII region.

The pressure confined wind of the massive and compact superstar cluster M82-A1