The detection of synchrotron radio emission from jets
powered by massive protostars indicates the presence of relativistic electrons and magnetic fields of strength $\sim$0.3$-$5~mG. We study diffusive shock acceleration and
magnetic field amplification in protostellar jets with speed
1000 km s$^{-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$^{-1}$.
Cosmic ray acceleration and gamma-ray emission from protostellar jets
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Pre-published on:
July 10, 2021
Published on:
March 18, 2022
Abstract
DOI: https://doi.org/10.22323/1.395.0684
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Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
Copyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.