AbstractWe review recent progress in elucidating the relationship between high-energy radiation and the interstellar medium (ISM) in young supernova remnants (SNRs) with ages of ∼2000 yr, focusing in particular on RX J1713.7−3946 and RCW 86. Both SNRs emit strong nonthermal X-rays and TeV $\gamma $
γ
-rays, and they contain clumpy distributions of interstellar gas that includes both atomic and molecular hydrogen. We find that shock–cloud interactions provide a viable explanation for the spatial correlation between the X-rays and ISM. In these interactions, the supernova shocks hit the typically pc-scale dense cores, generating a highly turbulent velocity field that amplifies the magnetic field up to 0.1–1 mG. This amplification leads to enhanced nonthermal synchrotron emission around the clumps, whereas the cosmic-ray electrons do not penetrate the clumps. Accordingly, the nonthermal X-rays exhibit a spatial distribution similar to that of the ISM on the pc scale, while they are anticorrelated at sub-pc scales. These results predict that hadronic $\gamma $
γ
-rays can be emitted from the dense cores, resulting in a spatial correspondence between the $\gamma $
γ
-rays and the ISM. The current pc-scale resolution of $\gamma $
γ
-ray observations is too low to resolve this correspondence. Future $\gamma $
γ
-ray observations with the Cherenkov Telescope Array will be able to resolve the sub-pc-scale $\gamma $
γ
-ray distribution and provide clues to the origin of these cosmic $\gamma $
γ
-rays.
Cosmic-Ray Transport, Energy Loss, and Influence in the Multiphase Interstellar Medium