- Conference date: 8–10 October 2008
- Location: Abano Terme (Italy)
Colliding winds of massive stars in binary systems are viable candidates for non‐thermal high‐energy photon emission. Long since, coincidences between massive star systems/associations and γ‐ray sources have been noted. Now, with the sensitivity of the Fermi Gamma Ray Observatory and current very‐high‐energy (VHE) Cherenkov instruments, will it be possible to sensibly probe these systems as high‐energy emitters.
We will summarize the characteristics and broadband predictions of generic optically thin emission models in the observables accessible at GeV and TeV energies. The ability to constrain orbital parameters of massive star‐star binaries through GeV‐to‐TeV observations is discussed. As an example we will present orbital parameter constraints for the nearby Wolf‐Rayet binary system WR 147 based on recently published VHE flux limits. Combining our broadband emission model with the cataloged binaries systems and their individual parameters allows us to conclude on the population of massive star‐star systems at high‐energy γ‐rays.
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