A weakly magnetized (similar to 10(7) G) neutron star, slowly spun up by ac
cretion in an X-ray binary, crosses the instability boundary for r-mode ins
tability at P = 1-2 msec. The amplitude of the oscillation, which initially
increases only at the spinup time scale, is secularly unstable due to the
negative temperature dependence of the viscosity in neutron star matter, an
d diverges after a few hundred years. Angular momentum loss by the gravitat
ional wave causes strong differential rotation, in which the magnetic field
is wound up to 10(17)G On a time scale of a few months. When this held bec
omes unstable to buoyancy instability, a surface field strength of a few 10
(16)G is produced on a TEM = time scale of seconds, which then powers a GRB
with energies of 10(51)-10(52) and duration of 1-100 sec.