A detailed study of the magnetic field data from both Voyager 1 and 2 has revealed interesting properties of the near and distant Jovian magnetotail. During the first encounter, when Voyager 1 passed between 80 and 140 RJ from Jupiter in the near tail and was almost entirely in the northern lobe magnetic field, the field lines were slightly twisted into a right-handed helix with pitch angle of about 2¿-3¿. The frequency spectrum of magnetic fluctuations in this region does not appear to be turbulent. A slight tendency of the magnetic field in the distant magnetotail to twist in a right-hand sense in the northern lobe and left-hand in the southern lobe is found as far as 7500 RJ downstream in Voyager 2 data. At nearly 7000 RJ the spacecraft was apparently in the magnetosheath near the tail magnetopause, and a 5.3-hour periodicity in the magnetic field was seen. The magnetic spectra of the distant tail encounters from 6000 to 7500 RJ have power law indices of f-5/3, identical to that of solar wind magnetic field spectra at these distances. It is possible that the distant tail magnetic fields have become turbulent, or that solar wind fields from the magnetosheath have diffused into the tail. During one event an interplanetary sector crossing was observed in Voyager 1 solar wind data, as predicted by Kurth et al. (1982). This supports their conjecture that the tail had disconnected from Jupiter. The distant tail spectra from Voyager 2 are also compared with similar spectra obtained from Voyager 1 when it was in near radial alignment with Voyager 2. Limitations of the use of the spectral analysis algorithm in the very low density regions of the Jovian tail also are discussed.