1999A&A...341L...1S

A weakly magnetized (∼10⁷G) neutron star, slowly spun up by accretion in an X-ray binary, crosses the instability boundary for r-mode instability at P=1-2msec. 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, and diverges after a few hundred years. Angular momentum loss by the gravitational wave causes strong differential rotation, in which the magnetic field is wound up to 10¹⁷G on a time scale of a few months. When this field becomes unstable to buoyancy instability, a surface field strength of a few 10¹⁶G is produced on a time scale of seconds, which then powers a GRB with energies of 10⁵¹-10⁵² and duration of 1-100sec.