Magnetospheric Tails in the Solar Planetary System

Magnetospheric tails resulting from the interaction of a celestial body moving relative to the ambient magnetized plasma are discussed. A hydromagnetic model of a long planetary tail is presented. The tail is assumed to be a long structure in pressure equilibrium with the solar wind and with a partially open boundary. The model describes the basic properties (size, lobe, magnetic field, and plasma density) of the quiet distant terrestrial and jovian magnetotails as seen in the ISEE-3/and Voyager-1 data (at distances 200 Earth radii and 6000 Jupiter radii correspondingly behind the planets).