Constraining the coherence scale of the interstellar magnetic field using TeV gamma-ray observations of supernova remnants
Abstract
Galactic cosmic rays are believed to be accelerated at supernova remnant (SNR) shocks. In the hadronic scenario the TeV gamma-ray emission from SNRs originates from decaying pions that are produced in collisions of the interstellar gas and cosmic rays. Using cosmic ray magnetohydrodynamic simulations performed with the code AREPO, we show that magnetic obliquity-dependent shock acceleration is able to reproduce the observed TeV gamma-ray morphology of SNRs solely by varying the magnetic field topology. This allows us to constrain the magnetic coherence scale in the cases of SN1006 and Vela Jr shown here respectively to >200^(+10)_(-60) pc and 8^(+15)_(-6) pc.
- Publication:
-
Supernova Remnants: An Odyssey in Space after Stellar Death II
- Pub Date:
- June 2019
- Bibcode:
- 2019sros.confE.120P