A planetary magnetosphere, formed by the interaction of the solar wind with a planet’s global magnetic field (intrinsic) or upper atmosphere (induced), plays a significant role in both the neutral and ionized regimes of the local space environment. The structure and dynamics of the Terrestrial magnetospheres have many similarities and differences. Mercury and Earth offer examples of intrinsic magnetospheres that experience different degrees of solar wind forcing and atmospheric contributions. The induced magnetospheres of Venus and Mars depict the solar wind-atmospheric interaction with differences in ionospheric densities and the existence of remnant crustal magnetic fields, for instance. Similar plasma processes exist among these magnetospheres, but offer drastically different temporal and spatial scales (e.g., magnetic reconnection, ion escape, wave-particle interaction, flux rope formation). To provide a forum for discussion of recent data analysis and modeling efforts, we invite contributions on general magnetospheric processes at the Terrestrial planets. This includes, but is not limited to: solar wind-magnetosphere interactions, atmospheric escape, magnetosphere-ionosphere coupling, plasma acceleration and transport, magnetic reconnection, magnetotail dynamics, and bow shock physics. We strongly encourage comparative studies between planetary magnetospheres throughout the solar system. Results from various missions such as MESSENGER, BepiColombo, VEX, MMS, MEX, MGS, MAVEN, and more, are actively solicited.