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Non-thermal X-Ray Enhancement Around Dense Gas Clumps

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Shock-Cloud Interaction in RX J1713.7−3946

Part of the book series: Springer Theses ((Springer Theses))

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Abstract

RX J1713.7–3946 is a unique supernova remnant (SNR) emitting very high energy \(\gamma \)-rays and X-rays, which are likely emitted by cosmic ray particles accelerated in the SNR via diffusive shock acceleration. It has been suggested that the SNR’s shockwave interacts with the dense gas clumps around the SNR, affecting the synchrotron X-ray radiation and cosmic ray acceleration. However, to date, there has not been a quantitative study to clarify the connection among the X-rays, gas clumps, and accelerated cosmic ray electrons. In this Chapter, we show a strong connection between synchrotron X-rays and the surrounding gas distribution by comparing the spatial distribution among CO, HI, and X-rays over the entire SNR. The present work is aimed at better understanding the SNR shock interstellar gas interaction and thereby establishing the origin of the distribution of the synchrotron X-rays in the SNR RX J1713.7–3946.

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  1. Department of Physics, Nagoya University, Nagoya, Japan

    Hidetoshi Sano

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  1. Hidetoshi Sano
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Sano, H. (2017). Non-thermal X-Ray Enhancement Around Dense Gas Clumps. In: Shock-Cloud Interaction in RX J1713.7−3946. Springer Theses. Springer, Tokyo. https://doi.org/10.1007/978-4-431-55636-7_2

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