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Following work by W\"unsch and collaborators, we investigate aself-enrichment scenario for second generation star formation in globularclusters wherein wind material from first generation massive stars rapidlyradiatively cools. Radiative energy loss allows retention of fast winds withinthe central regions of clusters, where it fuels star formation. Secondary starformation occurs in $\sim3-5$ Myr, before supernovae, producing uniform ironabundances in both populations. We derive the critical criteria for radiativecooling of massive star winds and the second generation mass as a function ofcluster mass, radius, and metallicity. We derive a critical condition on $M/R$,above which second generation star formation can occur. We speculate that abovethis threshold the strong decrease in the cluster wind energy and momentumallows ambient gas to remain from the cluster formation process. We reproducelarge observed second generation fractions of $\sim30-80\%$ if wind materialmixes with ambient gas. Importantly, the mass of ambient gas required is onlyof order the first generation's stellar mass. Second generation heliumenrichment $\Delta Y$ is inversely proportional to mass fraction in the secondgeneration; a large second generation can form with $\Delta Y\sim0.001-0.02$,while a small second generation can reach $\Delta Y\sim0.16$. Like otherself-enrichment models for the second generation, we are not able tosimultaneously account for both the full range of the Na-O anticorrelation andthe second generation fraction.

Second Generation Stars in Globular Clusters from Rapid Radiative Cooling of Pre-Supernova Massive Star Winds