Non-thermal X-rays and interstellar gas toward the \gamma-ray supernova
  remnant RX J1713.7-3946: Evidence for X-ray enhancement around CO and HI
  clumps
  RX J1713.7-3946 is the most remarkable very-high-energy \gamma-ray supernova
remnant which emits synchrotron X-rays without thermal features. We made a
comparative study of CO, HI and X-rays in order to better understand the
relationship between the X-rays, and the molecular and atomic gas. The results
indicate that the X-rays are enhanced around the CO and HI clumps on a pc scale
but are decreased inside the clumps on a 0.1 pc scale. Magnetohydrodynamic
numerical simulations of the shock interaction with molecular and atomic gas
indicate that the interaction between the shock waves and the clumps excite
turbulence which amplifies the magnetic field around the clumps (Inoue et al.
2012). We suggest that the amplified magnetic field around the CO and HI clumps
enhances the synchrotron X-rays and possibly the acceleration of cosmic-ray
electrons.
