Magnetic tension in the tails of Titan, Venus and comet Halley

Magnetic tension in the tail of the classical induced magnetosphere produced by field line draping is directed downstream along the external plasma flow. This is confirmed by the calculation of tension in magnetospheres of Venus and comet Halley which are firmly established as celestial bodies with negligible magnetic field. On the contrary, magnetic field structure observed in numerous Cassini flybys in the region of Titan interaction with the corotating flow of Kronian magnetosheric plasma contradicts the classical picture of the ideal induced magnetosphere produced by magnetic field line draping about the obstacle. Clear draping is observed only upstream of the Titan, but not in the Titan magnetic wake. We consider the magnetic field tension downstream the Titan magnetic tail and show that the magnetic field direction is not consistent with the induced magnetosphere produced by magnetic field lines draping. We arrive at the conclusion that the mechanisms alternative to the induced magnetosphere formation should be considered for the Titan magnetic environment.