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For gamma-ray bursts (GRBs) born in a stellar wind, as the reverse shockcrosses the ejecta, usually the shocked regions are still precipitated by theprompt MeV \gamma-ray emission. Because of the tight overlapping of the MeVphoton flow with the shocked regions, the optical depth for the GeV photonsproduced in the shocks is very large. These high energy photons are absorbed bythe MeV photon flow and generate relativistic e^\pm pairs. These pairsre-scatter the soft X-ray photons from the forward shock as well as the prompt\gamma-ray photons and power detectable high energy emission, significant partof which is in the sub-GeV energy range. Since the total energy contained inthe forward shock region and the reverse shock region are comparable, thepredicted sub-GeV emission is independent on whether the GRB ejecta aremagnetized (in which case the reverse shock IC and synchrotron self-Comptonemission is suppressed). As a result, a sub-GeV flash is a generic signaturefor the GRB wind model, and it should be typically detectable by the future{\em Gamma-Ray Large Area Telescope} (GLAST). Overlapping also influenceneutrino emission. Besides the 10^{15} \sim 10^{17} eV neutrino emissionpowered by the interaction of the shock accelerated protons with thesynchrotron photons in both the forward and reverse shock regions, there comesanother $10^{14}$eV neutrino emission component powered by protons interactingwith the MeV photon flow. This last component has a similar spectrum to the onegenerated in the internal shock phase, but the typical energy is slightlylower.Comment: 7 pages, accepted for publication in Ap

Early Photon‐Shock Interaction in a Stellar Wind: A Sub‐GeV Photon Flash and High‐Energy Neutrino Emission from Long Gamma‐Ray Bursts