Our numerical simulations on the effects of gravito-electrodynamics on the positively charged dust grains of the D68 ringlet of Saturn’s D ring reveal that dust grains, measuring between 0.028 and 0.01 nanometers launched with Keplerian velocity in the equatorial plane, can maintain stable orbits around the planet for years. Slightly larger grains 0.029 n to 0.1n size descending onto Saturn's atmosphere. While grains ofsize between 1 micrometer and 0.11 nanometers intersect with D72, at, potentially contributing to the recycling of ring materials within the equatorial plane. However, when these dust grains are launched with initial speed same as the Saturn's rotation, they either fall towards the planet or are stably trapped as the Keplerian launch ones. Those between the sizes 03 to 0.1n stably orbit around the local magnetic field lines akin to the Keplerian-launched particles, but now in retrograde directions. Size between 1 micron and 0.04 nanometers move inward until they collide with Saturn's atmosphere.. In both the cases, those unstable grains moving towards and outwards the planet in a bouncing manner above and below the equatorial plane. The confinement of the dust motions to the equatorial plane offers a plausible explanation for the depletion of electrons and the conductivity enhancement observed in the equatorial region of Saturn's ionosphere. Dispersion of charged dust across longitudes highlights Lorentz force's role in segregating D rings by grain size. Those moving towards the planet are likely the observed in-falling material during Cassini's missions.