We performed direct N-body simulations to investigate the behavior of SMBH in axisymmetric galactic nuclei.The stars are distributed following a rotating King model with W =6 and ω= 0.3,0.6.We measured the tidal disruption(TD)rate in these systems,compared with that in spherical systems,and found a higher TD rate in axisymmetric systems.This can be explained by an extended loss-cone in phase space which is raised from the fact that angular momentum J is not conserved.We also found the distribution of the TD stars origin,i.e.the last apocenter position,are peaked at the so called critical radius.Due to the 2-dimension nature of the system,inside the influence radius rh,the origin of TD stars have angular dependence(zenith angle)– they are concentrated around the equatorial plane; while outside of the influence radius this dependence is weaker.Inside rh,most of stars are moving on two families of regular orbit,called SAT and saucer orbits.We show that these orbits are the key to explain the angular dependence of the TD stars origin.