; Wang, Xiang-Yu
; Yu, Yun-Wei] Nanjing Univ, Dept Astron, Nanjing 210093, Peoples R China
; [Yu, Yun-Wei] Huazhong Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China
; [Meszaros, Peter] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA
; [Meszaros, Peter] Penn State Univ, Dept Phys, University Pk, PA 16802 USA
; [Wang, Xiang-Yu] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China
The observations of gamma- ray bursts (GRBs) such as 980425, 031203 and 060218, with luminosities much lower than those of other classic bursts, lead to the definition of a new class of GRBs-LL-GRBs. The nature of the outflow responsible for them is not yet clear. Two scenarios have been suggested: one is the conventional relativistic outflow with initial Lorentz factor of order of Gamma(0) greater than or similar to 10 and the other is a trans-relativistic outflow with Gamma(0) similar or equal to 1-2. Here, we compare the high-energy gamma-ray afterglow emission from these two different models, taking into account both synchrotron self-inverse Compton (SSC) scattering and the external inverse Compton scattering due to photons from the cooling supernova or hypernova envelope (SNIC). We find that the conventional relativistic outflow model predicts a relatively high gamma-ray flux from SSC at early times (<10(4) s for typical parameters) with a rapidly decaying light curve, while in the trans-relativistic outflow model, one would expect a much flatter light curve of high-energy gamma- ray emission at early times, which could be dominated by both the SSC emission and the SNIC emission, depending on the properties of the underlying supernova and the shock parameter epsilon(e) and epsilon(B). The Fermi Gamma-ray Space Telescope should be able to distinguish between the two models in the future.