Can compact accelerators inject PeV cosmic rays in the interstellar medium?

Gamma-ray emitting binaries hosting a massive star are among the most efficient and powerful accelerators of the Galaxy. The closest vicinity of the binary is believed to be the region where electrons (and possibly protons and nuclei) are accelerated, reaching in some cases energies approaching 100 TeV. This implies that these sources are potential Pevatrons, in particular if protons and nuclei are also accelerated, as they are less affected by energy losses than electrons, close to the binary. However, once the particles are accelerated, they will have to propagate a large distance before reaching the interstellar medium (ISM), if they are to contribute to the Galactic cosmic rays. These particles may suffer adiabatic losses in the way, which would strongly reduce the energy at which they are injected in the ISM. This project aims at calculating the energy evolution of cosmic rays after being accelerated close to the binary system, and while they are transported by the powerful outflows emerging from those regions.