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Molecular and Atomic Gas in the Young TeV γ-Ray SNRs RX J1713.7–3946 and RX J0852.0–4622; Evidence for the Hadronic Production of γ-Rays

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Cosmic Rays in Star-Forming Environments

Part of the book series: Astrophysics and Space Science Proceedings ((ASSSP,volume 34))

Abstract

The interstellar molecular clouds are the site of star formation and also the target for the cosmic ray protons to produce γ-rays via the hadronic process. The interstellar atomic gas is enveloping the molecular clouds and may also be dense enough to affect the γ-ray production. In this chapter, some of the basic properties of the interstellar gas both in molecular and atomic forms will be reviewed. Then, it is presented that two young TeV γ-ray SNRs, RX J1713.7–3946 and RX J0852.0–4622, show good spatial correspondence between the γ-rays and the interstellar protons. The good spatial correspondence provides a support for the hadronic origin of the γ-rays in these SNRs. It is emphasized that both molecular and atomic hydrogen plays a role as targets for cosmic ray (CR) protons. The clumpy distribution of the target interstellar medium (ISM) protons is crucial in the interaction of the supernova shocks with the ISM, whereas models with uniform ISM distribution are not viable. Finally, it is suggested that the dense atomic gas without molecules may occupy the dominant part of the dark gas in the local ISM.

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Acknowledgements

The author is grateful to the SOC for inviting him to this most stimulating conference. He is grateful to all the collaborators in this project for their invaluable contributions. His special thanks are to Felix Aharonian, Gavin Rowell, Naomi M. McClure-Griffiths, Tsuyoshi Inoue and Shu-ichiro Inutsuka. NANTEN2 is an international collaboration of 10 universities; Nagoya University, Osaka Prefecture University, University of Cologne, University of Bonn, Seoul National University, University of Chile, University of New South Wales, Macquarie University, University of Sydney, and University of ETH Zurich. This work was financially supported by a grant-in-aid for Scientific Research (KAKENHI, No. 21253003, No. 23403001, No. 22540250, No. 22244014, No. 23740149, No. 22740119 and No. 24224005) from MEXT (the Ministry of Education, Culture, Sports, Science and Technology of Japan). This work was also financially supported by the Young Research Overseas Visits Program for Vitalizing Brain Circulation (R2211) and the Institutional Program for Young Researcher Overseas Visits (R29) by JSPS (Japan Society for the Promotion of Science) and by the grant-in-aid for Nagoya University Global COE Program, Quest for Fundamental Principles in the Universe: From Particles to the Solar System and the Cosmos, from MEXT.

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  1. Department of Physics, Nagoya University,Furo-cho, Chikusa-ku, Nagoya, 464-8601, Japan

    Yasuo Fukui

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  1. Yasuo Fukui
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Correspondence to Yasuo Fukui .

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  1. , (IEEC-CSIC) Campus UAB, Fac. de Ciències, ICREA & Institute of Space Sciences, Torre C5, parell, 2a planta, Barcelona, 08193, Spain

    Diego F. Torres

  2. , Leopold-Franzens-Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstraße 25/8, Innsbruck, 6020, Austria

    Olaf Reimer

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Fukui, Y. (2013). Molecular and Atomic Gas in the Young TeV γ-Ray SNRs RX J1713.7–3946 and RX J0852.0–4622; Evidence for the Hadronic Production of γ-Rays. In: Torres, D., Reimer, O. (eds) Cosmic Rays in Star-Forming Environments. Astrophysics and Space Science Proceedings, vol 34. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-35410-6_17

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  • DOI: https://doi.org/10.1007/978-3-642-35410-6_17

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