  The high energy neutrino signature from proton-proton and photo-meson
interactions in a supernova remnant shell ejected prior to a gamma-ray burst
provides a test for the precursor supernova, or supranova, model of gamma-ray
bursts. Protons in the supernova remnant shell, and photons entrapped from a
supernova explosion or a pulsar wind from a fast-rotating neutron star remnant
provide ample targets for protons escaping the internal shocks of the gamma-ray
burst to interact and produce high energy neutrinos. We calculate the expected
neutrino fluxes, which can be detected by current and future experiments.
