Structure of the inner debris disk composed of 3 × 10⁵ Ceres-like asteroids of mass 10⁻⁶ M_Jup on stable orbits, seen in the (a₀, e₀)-plane of Jacobian (canonical) osculating elements at the initial 1998.830 epoch. The colors of the asteroids indicate the lowest order MMR in which they are involved with HR 8799e, as indicated in the diagrams, or belong to the innermost, quasi-homogeneous disk (gray points) according to Fig. 10. The light gray curve indicates the collision of the orbits with HR 8799e and the red curve is an image of the collision curve shifted by Δa₀ ≃ 4 au toward the star. We note that loose points above the collision curve in the top panel represent immediately scattered asteroids on regular but hyperbolic (open) orbits.