Abstract
We propose that the chaotic stellar winds from massive stars are potential π 0 -decay γ-ray sources. A small fraction of the thermal ions is first-order Fermi accelerated to high energies by the shocks embedded in the highly unstable radiatively driven winds. These particles interact with the thermal ions to produce γ-rays peaked around 0.1 GeV via π 0 -decay. When the mass-loss rate of an early-type star is high enough, the wind becomes opaque to the ion-ion interactions and a substantial fraction of the nonthermal ions' energy is emitted in γ-rays
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