The role of the diffusive protons in the gamma-ray emission of SNR RX J1713.7-3946. Issue Volume 12:Issue S331(2017) (17th October 2017)

• Record Type: Journal Article
• Authors: Zhang, Xiao; Chen, Yang
• Editors: Marcowith, A.; Renaud, M.; Dubner, G.; Ray, A.; Bykov, A.
• Is Part Of: Proceedings of the International Astronomical Union. Volume 12:Issue S331(2017)
• Page Start: 304
• Page End: 309
• Publication Date: 2017-10-17
• Subjects: radiation mechanisms: nonthermal, -- ISM: individual (G347.3−0.5), -- (ISM:) supernova remnants, -- gamma rays: theory; Astronomy -- Congresses; Astronomy -- Periodicals; 520
• DOI: 10.1017/S1743921317004355
• Languages: English
• ISSNs: 1743-9213

Abstract

Abstract: RX J1713.7-3946 is a prototype in the γ-ray-bright supernova remnants (SNRs) and is in continuing debates on its hadronic versus leptonic origin of the γ-ray emission. We explore the role played by the diffusive relativistic protons that escape from the SNR shock wave in the γ-ray emission, apart from the emission of high energy particles from the inside of the SNR. In the scenario that the SNR shock propagates in a clumpy molecular cavity, we consider that the γ-ray emission from the inside of the SNR may either arise from the IC scattering or from the interaction between the trapped energetic protons and the shocked clumps. The dominant origin between them depends on the electron-to-proton number ratio. The surrounding molecular cavity wall is considered to also produce γ-ray emission due to the "illumination" by the diffusive protons that escaped from the shock wave during the expansion history. The broad-band spectrum can be well explained by this two-zone model, in which the γ-ray emission from the inside governs the TeV band, while the outer emission component substantially contributes to the GeV γ-rays. The two-zone model can also explain the TeV γ-ray radial brightness profile that significantly stretches beyond the nonthermal X-ray emitting region.