  We present a numerical simulation of the dynamical interaction between the
proposed Planet Nine and a debris disk around the Sun for $4{\rm Gyr}$,
accounting for the secular perturbation of the four giant planets in two
scenarios: (a) an initially thin circular disk around the Sun (b) inclined and
eccentric disk. We show, in both scenarios, that Planet Nine governs the
dynamics in between $1000{\rm -5000{\rm AU}}$ and forms spherical structure in
the inner part ($\sim1000{\rm AU}$) and inclined disk. This structure is the
outcome of mean motion resonances and secular interaction with Planet Nine. We
compare the morphology of this structure with the outcome from a fly-by
encounter of a star with the debris disk and show distinct differences between
the two cases. We predict that this structure serves as a source of comets and
calculate the resulting comet production rate to be detectable.
