Nonthermal Emission from a Supernova Remnant in a Molecular Cloud

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Reionization by Hard Photons. I. X-Rays from the First Star Clusters (2000, background): “However, this is somewhat model-dependent : in models where electrons are injected directly from the thermal pool, D5% of the energy in the shock must go to nonthermal electrons in order to match gamma-ray observations (Bykov et al. 2000).”
Limits on diffusive shock acceleration in supernova remnants in the presence of cosmic-ray streaming instability and wave dissipation (2003, background): “Different aspects of particle acceleration by supernova shocks moving in partly ionized interstellar gas were also considered by Boulares & Cox (1988), Bykov et al. (2000).”
OBSERVATION OF SUPERNOVA REMNANT IC 443 WITH THE FERMI LARGE AREA TELESCOPE (2010, methodology): “…but before the discoveries of the PWN (Olbert et al. 2001) and MAGIC source (Albert et al. 2007), models have been proposed to explain the emission between ∼5 keV and ∼5 GeV by bremsstrahlung in dense clouds (e.g., Bykov et al. 2000) with possible mix of synchrotron (e.g., Sturner et al. 1997).”
Superbubbles and energetic particles in the Galaxy. I. Collective effects of particle acceleration (2004, background): “…scale hydrodynamic motions with velocities close to the Alfvén speed (cascading to smaller scales down to the gyroradius of thermal protons; e.g. Goldreich & Sridhar 1997), relativistic particles can generate or amplify MHD waves notably through streaming instability (see e.g. Bykov et al. 2000).”