Winds Driven by Super Star Clusters: The Self‐Consistent Radiative Solution

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Abstract
Here we present a self-consistent stationary solution for spherically symmetric winds driven by massive star clusters under the impact of radiative cooling. We demonstrate that cooling may drastically modify the distribution of temperature if the rate of injected energy approaches a critical value. We also prove that the stationary wind solution does not exist when the energy radiated away at the star cluster center exceeds ~30% of the energy deposition rate. Finally, we thoroughly discuss the expected appearance of super star cluster winds in the X-ray and visible line regimes. The three solutions found, the quasi-adiabatic, the strongly radiative wind, and the inhibited stationary solution, are then compared to the winds from the Arches cluster, the NGC 4303 central cluster, and to the supernebula in NGC 5253.
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