Analyses of Voyager magnetic field measurements have extended our understanding of the structural and temporal characteristics of Jupiter's magnetic tail. The magnitude of the magnetic field in the lobes of the tail is found to decrease with Jovicentric distance approximately as r-1,4, compared with the power law exponent of -1.7 found for the rate of decrease along the Pioneer 10 outbound trajectory. Voyager observations of magnetic field component variations with distance from the magnetic dipole axis are consistent with the variations expected from the geometry of a magnetotail field and hence do not unambiguously support the uniform radial plasma outflow model derived from Pioneer 10 data. Voyager 2 has shown that the azimuthal current sheet which surrounds Jupiter in the inner and middle magnetosphere extends 'tailward' (in the antisun direction) to a distance of at least 100 RJ. In the tail this current sheet consists of a plasma sheet and embedded 'neutral' sheet. In the region of the tail where the sheet is observed, the variation of the magnetic field as a result of the sheet structure and its 10-hour periodic motion is the dominant variation seen. Studies of both the large-scale configuration of the current sheet viewed as a surface and of the internal structure of the sheet and its orientation indicated that (1) at distances >30 RJ in the tail the sheet is oriented within ¿10¿ of the Jovian equatorial plane, most likely as a result of the solar wind interaction with the Jovian magnetosphere, (2) the surface moves north and south with an amplitude of several RJ with respect to that plane, and (3) at large distances this motion is primarily due to a rocking of the current sheet about the Jupiter-sun line. A mathematical model that takes the tail geometry into account provides a simpler description of sheet motion in the deep tail than do models based on axial symmetry. The plasma sheet in the tail is estimated to have an average thickness of ?5 RJ.