Cosmic ray acceleration and gamma-ray emission from protostellar jets
Résumé
The detection of synchrotron radio emission from jetspowered by massive protostars indicates the presence of relativistic electrons and magnetic fields of strength $\sim$0.3$-$5~mG. We study diffusive shock acceleration andmagnetic field amplification in protostellar jets with speed1000 km s$^{-1}$. We show that the magnetic field in the synchrotron emitter can be amplified by the non-resonant hybrid (Bell) instability excited by the cosmic-ray streaming. By combining the synchrotron data with basic theory of Bell instability we estimate the magnetic field in the synchrotron emitter and the maximum energy of protons.Protons can achieve maximum energies $\sim 0.1$ TeV and emit $\gamma$ rays in their interaction with matter fields. We predict detectable levels of $\gamma$ rays in IRAS~16547-5247 and IRAS~16848-4603.The detection of this radiation by the Fermi satellite in the GeV domain and the forthcoming Cherenkov Telescope Array at higher energies may open a new window to study the formation of massive stars, as well as diffusive acceleration and magnetic field amplification in shocks with velocities of about 1000 km s$^{-1}$.