Inverse Compton emission from a cosmic-ray precursor in RX J1713.7−3946

Citations of this article
Mendeley users who have this article in their library.


Recently, the High Energy Stereoscopic System (H.E.S.S.) reported two new interesting results for a γ-ray emitting supernova remnant, RX J1713.7−3946 (G347.3−0.5). The first result is the establishment of a broken power-law spectrum of GeV–TeV γ-rays. The other is a more extended γ-ray spatial profile than the one in the X-ray band. In this paper, we show both of these results can be explained by inverse Compton emission from accelerated electrons. If the maximum energy of electrons being accelerated decreases with time, the broken power-law spectrum can be generated by accumulation. Furthermore, the extended component of γ-ray profile can be interpreted as a CR precursor of currently accelerated electrons.




Ohira, Y., & Yamazaki, R. (2017). Inverse Compton emission from a cosmic-ray precursor in RX J1713.7−3946. Journal of High Energy Astrophysics, 1314, 17–21.

Register to see more suggestions

Mendeley helps you to discover research relevant for your work.

Already have an account?

Save time finding and organizing research with Mendeley

Sign up for free