Analyses using data from the plasma wave, plasma science, planetary radio astronomy, and magnetometer experiments onboard Voayager 2 covering the period October 1980 to August 1981 are shown to provide compelling evidence for and characteristics of a Jovian magnetotail extending at least to 9000 Jovian radii from the planet. Voyager 1 magnetic field and wave data from the same time period indicate that it was very unlikely that the distant Jovian tail was observed at that spacecraft. During approximately (25-day) periodic sightings of the tail by Voyager 2 the magnetic field tended to point radially towards or away from Jupiter, indicating preservation to large distances of the bipolar, lobelike structure observed ner the planet, as in the earth's case. This periodicity, along with various properties of the solar wind at this time, indicates that the tail is apparently influenced by recurrent solar wind features. Anomalous magnetic fields, not aligned with the nominal tail axis, also exist within the tail especially in the low-density, ''central'' (core) region, indicating some complexity of internal structure. Approximately centered at each of the tail encounter periods we see broad-scale plasma velocity, density, and field magnitude decreases; the latter are not expected for a quasi-steady tail structure but probably indicate tail expansion to the position of the spacecraft. On a finer scale the field increases across the inbound boundary as expected for an outward pressure imbalance. We argue that a possible contributer to the internal pressure of the tail is a considerable amount of tailward flowing plamsa in addition to the expected internal field pressure. Magnetic field invariance analyses provide quantitative evidence for field line draping around the boundary of the tail and also show that internal tail field transverse variations occur. We suggest that the Jovian tail has a quasi-periodically variable width (resembling of string of sausages) on a very long-length scale, tens of thousands of Jupiter radii, due to the influence of the ≈25-day radial variation of the solar wind pressure. The tail is also apparently filamentary to some degree.