We 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 \(\gamma \)-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 \(\gamma \)-rays can be emitted from the dense cores, resulting in a spatial correspondence between the \(\gamma \)-rays and the ISM. The current pc-scale resolution of \(\gamma \)-ray observations is too low to resolve this correspondence. Future \(\gamma \)-ray observations with the Cherenkov Telescope Array will be able to resolve the sub-pc-scale \(\gamma \)-ray distribution and provide clues to the origin of these cosmic \(\gamma \)-rays.

我们回顾了阐明高能辐射与年龄约 2000 年的年轻超新星遗迹 (SNR) 中的星际介质 (ISM) 之间关系的最新进展，特别关注 RX J1713.7-3946 和 RCW 86。两个 SNR发射强非热 X 射线和 TeV \(\gamma \)射线，它们包含星际气体的块状分布，其中包括原子氢和分子氢。我们发现冲击云相互作用为 X 射线和 ISM 之间的空间相关性提供了可行的解释。在这些相互作用中，超新星冲击撞击典型的 pc 级致密核心，产生高度湍流的速度场，将磁场放大至 0.1-1 mG。这种放大导致团块周围的非热同步辐射增强，而宇宙射线电子不会穿透团块。因此，非热 X 射线在 pc 尺度上表现出与 ISM 相似的空间分布，而它们在亚 pc 尺度上是反相关的。这些结果预测强子\(\gamma \)射线可以从密集的核心发射，导致\(\gamma \)射线和 ISM之间的空间对应。\(\gamma \)射线观测的当前 pc 尺度分辨率太低，无法解决这种对应关系。未来使用切伦科夫望远镜阵列进行的\(\gamma \)射线观测将能够解决亚 pc 级\(\gamma \)射线分布并提供这些宇宙\(\gamma \)起源的线索-射线。