Abstract
Two high energy radiation mechanisms, i.e., the electron inverse Compton emission and the proton synchrotron emission, as well as their relative importance with respect to the electron synchrotron emission, are explored in the context of gamma-ray burst afterglow theories, with the focus on the possible signatures of these emission components in the broad-band spectra and in the GeV to keV light curves of gamma-ray burst afterglows. A general conclusion is that the electron inverse Compton emission dominated parameter regime is the most favorable regime for the high energy emission, and the inverse Compton component is detectable by GLAST within hours for bursts at typical cosmological distances, and by Chandra in days if the ambient density is high.
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