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Abstract
We present solutions for the structure and evolution of bubbles created by slow stellar winds, during their fully and partially radiative phases. Exact limiting forms are derived for the partially radiative case, and the transition between the two phases is analysed under the assumption of steady spherical flow. We compute the factor by which the bubble's radial momentum is amplified relative to that of the wind, and provide accurate formulae for its expansion across the fully-to-partially radiative transition. Our results will be useful in the study of protostellar outflow cocoons and bubbles driven by mass-loaded winds from star clusters.
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