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We study high‐energy gamma‐ray afterglow emission from gamma‐ray bursts (GRBs) in the prior emission model, which is proposed to explain the plateau phase of the X‐ray afterglow. This model predicts the high‐energy gamma‐ray emission when the prompt GRB photons from the main flow are up‐scattered by relativistic electrons accelerated at the external shock due to the prior flow. The expected spectrum has the peak of  ∼10–100  GeV at around the end time of the plateau phase for typical GRBs, and high‐energy gamma‐rays from nearby and/or energetic GRBs can be detected by the current and future Cherenkov telescopes such as MAGIC, VERITAS, CTA and possibly  Fermi . Multiwavelength observations by ground‐based optical telescopes as well as  Fermi  and/or  Swift  satellites are important to constrain the model. Such external inverse‐Compton emission may even lead to GeV–TeV gamma‐ray signals with the delay time of  ∼10–100  s, only if the plateau phase is short lived.

High‐energy emission as a test of the prior emission model for gamma‐ray burst afterglows