  In the present article, we study the orbital resonance corresponds to an
extended object approximated up to the dipole order term in Kerr spacetime. We
start with the Mathisson-Papapetrou equations under the linear spin
approximation and primarily concentrate on two particular events. First, when
the orbits are nearly circular and executing a small oscillation about the
equatorial plane and second, a generic trajectory confined on the equatorial
plane. While in the first case, all the three fundamental frequencies, namely,
radial $\Omega_r$, angular $\Omega_{\theta}$, azimuthal $\Omega_{\phi}$ can be
commensurate with each others and give rise to the resonance phenomenon, the
later is only accompanied with the resonance between $\Omega_r$ and
$\Omega_{\phi}$ as we set $\theta=\pi/2$. We provide a detail derivation in
locating the prograde resonant orbits in either of these cases and also study
the role played by the spin of the black hole. The implications related to
spin-spin interactions between the object and black hole are also demonstrated.
