  The gamma-ray burst (GRB) model for production of ultra-high-energy
cosmic-rays (UHECRs) is based on the hypothesis that GRBs arise from the
dissipation of the kinetic energy of relativistic fireballs at cosmological
distances. Recent GRB afterglow observations support the validity of this
hypothesis and provide quantitative support for the model. The inferred
physical fireball parameters imply that protons may be accelerated to >10^20
eV, and the inferred GRB energy generation rate is similar to that required to
account for the observed flux of UHECRs.
  Strong suppression of UHECR flux is expected in this model above 10^19.7 eV,
due to proton interaction with CMB photons. Strong deviations from model flux
derived under the assumption of uniform source distribution is expected above
10^20 eV, due to source clustering. The flux above 10^20.5 eV is expected to be
dominated by few, narrow spectrum sources. While model predictions can not be
tested (with high confidence level) at present, the predicted signatures should
be observed with the planned Auger and Telescope-Array UHECR detectors.
  A natural consequence of the GRB model of UHECR production is the conversion
of a large fraction, ~10%, of the fireball energy to accompanying burst of
\~10^14 eV and ~10^18 eV neutrinos. A km^2 neutrino detector would observe
several tens of events per year correlated with GRBs, and test for neutrino
properties (e.g. flavor oscillations, for which upward moving tau's would be a
unique signature, and coupling to gravity) with an accuracy many orders of
magnitude better than is currently possible.
