摘要
We present a possible hadronic explanation of the high-energy γ-ray emission from two very high-energy （VHE） sources, HESS 31745-303 （A ） and HESS 31714-385, which coincide with supernova remnants （SNRs） interacting with dense molecular clouds （MCs）. We calculate the proton spectra and the corresponding hadronic γ-ray spectra for different Mach numbers of the shock wave in a semi-analytical model for the non-linear shock acceleration process, then apply the model to the two newly discovered TeV sources. The results show that the γ-ray spectra for the two sources with energies above 100 MeV detected by HESS and EGRET can be reproduced with low Mach numbers about 2.5. Thus the high-energy γ-ray origin for each one of the two sources can be interpreted as proton-proton （p-p） collisions in MCs overtaken by an SNR shock wave.
We present a possible hadronic explanation of the high-energy γ-ray emission from two very high-energy （VHE） sources, HESS 31745-303 （A ） and HESS 31714-385, which coincide with supernova remnants （SNRs） interacting with dense molecular clouds （MCs）. We calculate the proton spectra and the corresponding hadronic γ-ray spectra for different Mach numbers of the shock wave in a semi-analytical model for the non-linear shock acceleration process, then apply the model to the two newly discovered TeV sources. The results show that the γ-ray spectra for the two sources with energies above 100 MeV detected by HESS and EGRET can be reproduced with low Mach numbers about 2.5. Thus the high-energy γ-ray origin for each one of the two sources can be interpreted as proton-proton （p-p） collisions in MCs overtaken by an SNR shock wave.
基金
Supported by the National Natural Science Foundation of China under Grant Nos 10425314, 10778702 and 10778726, and the National Basic Research Programme of China under Grant No 2009CB824800.
