Leptonic Origin of TeV Gamma-Ray Emission from Crab Nebula
ZHANG Li1,2, WEI Bing-Tao2, FANG Jun1
1Department of Physics, Yunnan University, Kunming 6500912National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming 650011
Leptonic Origin of TeV Gamma-Ray Emission from Crab Nebula
ZHANG Li1,2;WEI Bing-Tao2;FANG Jun1
1Department of Physics, Yunnan University, Kunming 6500912National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, PO Box 110, Kunming 650011
摘要We study the nonthermal emission of the Crab nebula in the bands from radio to TeV γ-ray on a simplified time-dependent injection model. In this model, relativistic electrons in the Crab nebula consists of two components and their injected spectrum is a broken power law with different indices and a break energy. The relativistic electrons emit nonthermal photons through synchrotron and inverse Compton scattering off soft photon fields inside the nebula. The resulting spectrum calculated with the model is well consistent with the observed data ranging from radio to very high energy γ-rays for the Crab nebula, where the emission from radio to medium γ-rays is from electron's synchrotron emission, whereas the emission above ～100MeV primarily comes from the inverse Compton scattering of the relativistic electrons on synchrotron photons.
Abstract：We study the nonthermal emission of the Crab nebula in the bands from radio to TeV γ-ray on a simplified time-dependent injection model. In this model, relativistic electrons in the Crab nebula consists of two components and their injected spectrum is a broken power law with different indices and a break energy. The relativistic electrons emit nonthermal photons through synchrotron and inverse Compton scattering off soft photon fields inside the nebula. The resulting spectrum calculated with the model is well consistent with the observed data ranging from radio to very high energy γ-rays for the Crab nebula, where the emission from radio to medium γ-rays is from electron's synchrotron emission, whereas the emission above ～100MeV primarily comes from the inverse Compton scattering of the relativistic electrons on synchrotron photons.
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2007, Vol. 24 
