Hadronic Interpretation of the High-energy Gamma-ray Emission from W28
Observations of CO emission and OH masers on the supernova remnant (SNR) W28 indicate that the SNR interacts with molecular clouds (MCs) and very high-energy (VHE) observations with HESS and the reanalysis of the EGRET data for the remnant have been reported recently. The association of the VHE emission with MCs favors a possible hadronic origin of the TeV γ-rays; however, the γ-ray spectrum can not be well fitted with the usual proton index of ～ 2.0. Based on a semi analytical approach to the non-linear shock acceleration process, the proton spectrum can be calculated and then the corresponding hadronic γ-rays from proton-proton (p p) interactions can be investigated. We find that the high-energy γ-ray spectrum for W28 can be marginally reproduced with a low Mach number ~ 2.5.
acceleration of particles - gamma rays theory - ISM clouds - ISM individual (W28) - radiation mechanisms non-thermal
Jun Fang Li Zhang
Department of Physics, Yunnan University, Kunming, China
国际会议
The 10th Asian-Pacific Regional International Astronomical Union Meeting(第十届亚洲及太平洋地区天文学大会 APRIM)
昆明
英文
216-217
2008-08-03（万方平台首次上网日期，不代表论文的发表时间）