Particle acceleration and magnetic field amplification in massive young stellar object jets
Date Issued
2021
Author(s)
Abstract
Synchrotron radio emission from non-relativistic jets powered by massive protostars has been reported, indicating the presence of relativistic electrons and magnetic fields of strength ~0.3-5 mG. We study diffusive shock acceleration and magnetic field amplification in protostellar jets with speeds between 300 and 1500 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 in the range 0.04-0.65 TeV and emit γ rays in their interaction with matter fields. We predict detectable levels of γ rays in IRAS 16547-5247 and IRAS 16848-4603. The γ ray flux can be significantly enhanced by the gas mixing due to Rayleigh-Taylor instability. 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.
Volume
504
Issue
2
Start page
2405
Issn Identifier
0035-8711
Ads BibCode
2021MNRAS.504.2405A
Rights
open.access
File(s)![Thumbnail Image]()
![Thumbnail Image]()
Loading...
Name
2102.11583.pdf
Description
postprint
Size
849.92 KB
Format
Adobe PDF
Checksum (MD5)
b1260642ed903184e71071429b7b4375
Loading...
Name
stab635.pdf
Description
Pdf editoriale
Size
845.51 KB
Format
Adobe PDF
Checksum (MD5)
1341e94d2e58b60d4f5f38dc4b4a0b55