Mass fluxes for O-type supergiants with metallicity Z = Z/5
Abstract
A code used previously to predict O-star mass fluxes as a function of metallicity is used to compute a grid of models with the metallicity of the Small Magellanic Cloud (SMC). These models allow mass-loss rates to be derived by interpolation for all O-type supergiants in the SMC, with the possible exception of extremely massive stars close to the Eddington limit.
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