  We consider the problem of tidal disruption of stars in the centre of a
galaxy containing a supermassive binary black hole with unequal masses. We
assume that over the separation distance between the black holes the
gravitational potential is dominated by the more massive black hole. Also, we
assume that the number density of stars is concentric with the primary black
hole and has a power law cusp.We show that the bulk of stars with a small
angular-momentum component normal to the black hole binary orbit can reach a
small value of total angular momentum through secular evolution in the
gravitational field of the binary, and hence they can be tidally disrupted.
This effect is analogous to the so-called Kozai effect (Kozai, 1962, Lidov,
1961,1962) well known in celestial mechanics. We develop an analytical theory
of secular evolution of the stellar orbits and calculate the rate of tidal
disruption. We confront our analytical theory with a simple numerical model and
find very good agreement.
  Our results show that for primary black-hole mass \sim
10^{6}-10^{7}M_{\odot}, the black- hole mass ratio q > 10^{-2}, cusp size \sim
1pc, the tidal disruption rate can be as large as \sim 10^{-2}-1M_{\odot}/yr.
This is at least 10^{2}-10^{4} times larger than estimated for the case of a
single supermassive black hole. The duration of the phase of enhanced tidal
disruption is determined by the dynamical friction time scale, and it is rather
short: \sim 10^{5}yr. The dependence of the tidal disruption rate on the mass
ratio, as well as on the size of the cusp, is also discussed.
