  We explore the rates of tidal disruption events (TDEs) of stars by
supermassive black holes (SBHs) in galactic nuclei formed in mergers followed
by a formation and coalescence of a binary SBH. Such systems initially have a
deficit of stars on low-angular-momentum orbits caused by the slingshot process
during the binary SBH stage, which tends to reduce the flux of stars into the
SBH compared to the steady-state value. On the other hand, a newly formed
galactic nucleus has a non-spherical shape which enhances the mixing of stars
in angular momentum and thus the TDE rate. In galaxies with relatively low SBH
masses (<10^7 Msun), relaxation times are short enough to wash out the
anisotropy in initial conditions, and for more massive SBH the enhancement of
flux due to non-sphericity turns out to be more important than its suppression
due to initial anisotropy. Therefore, the present-day TDE rates generally
exceed conventional steady-state estimates based on a spherical isotropic
approximation. We thus conjecture that the lower observationally inferred TDE
rates compared to theoretical predictions cannot be attributed to the depletion
of low-angular-momentum stars by SBH binaries.
