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The detection of very-high-energy (VHE) gamma-ray emission in the afterglows of long-duration gamma-ray bursts (GRBs) has opened a new window into understanding these energetic cosmic phenomena. Among these, GRB 221009A stands out as the most energetic GRB ever observed, with TeV emission detected by the Large High Altitude Air Shower Observatory (LHAASO) in the 0.2–7 TeV energy band. The physical mechanisms responsible for such emission remain a topic of significant interest, particularly in the context of extreme particle acceleration and radiative processes.
We explored the afterglow emission of GRB 221009A using a hybrid model. In this framework, the VHE gamma-ray emission is attributed to the proton-synchrotron process, while the lower-energy radiation from optical to X-rays is explained by synchrotron radiation from electrons. By analyzing the observed data, we constrain the physical conditions of the GRB environment and investigate the implications for particle acceleration and energy partitioning in the relativistic shock. Our findings support the proton-synchrotron process as a promising mechanism for TeV afterglow emission, offering new insights into the interplay of particle populations and magnetic fields in GRB environments.
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