{"paper":{"title":"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","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"A. Kawamura, A. Mizuno, H. Horachi, H. Matsumoto, H. Sano, H. Yamamoto, J. Sato, K. Tachihara, K. Torii, N. Mizuno, R. Yamazaki, S. Inutsuka, S. Yoshiike, T. Fukuda, T. Hayakawa, T. Inoue, T. Kuwahara, T. Okuda, T. Onishi, T. Tanaka, Y. Fukui","submitted_at":"2013-04-29T17:43:31Z","abstract_excerpt":"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 cl"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1304.7722","kind":"arxiv","version":3},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}