Mars, characterized as a “desert” planet with little water vapor, primarily relies on dry deposition processes for dust removal. Although dry deposition processes include gravitational sedimentation, turbulent transfer, Brownian diffusion, impaction, and interception, gravitational sedimentation is considered the only way for dust removal in most current models. To have a more comprehensive understanding of the effects of Martian dust removal processes, a physics-based scheme of dry deposition processes (e.g., turbulent transfer, Brownian diffusion, impaction, and interception) with resolved dust particle sizes representing the lifting dust size distribution is implemented in the MarsWRF general circulation model in this study. The model results reveal that the dry deposition velocity increases significantly with the decrease in dust size, especially for small dust particles. This enhancement in the removal efficiency of small particles leads to an increase in the effective particle radius of airborne dust and a decrease in dust opacity, particularly in the high latitudes of the northern hemisphere during the period of high dust loading. In these latitudes, the atmospheric temperature rises from the surface up to an altitude of 55 km, with a peak temperature difference of about 3.8 K, driven by dynamical warming from the strengthened descending branch of the upper meridional circulation. In addition, the sublimation of CO2 surface ice in the high latitudes of the northern hemisphere is increased, and the condensation of the gas phase is decreased.