Magnetic properties of Jupiter's tail at distances from 80-7500 Jovian radii

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19860019428.pdf (2.3 MB)

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https://ntrs.nasa.gov/citations/19860019428

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http://hdl.handle.net/11603/30527

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UMBC Goddard Planetary Heliophysics Institute (GPHI)

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https://orcid.org/0000-0002-5317-988X

Date

1984-09-01

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Techical reports
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Citation of Original Publication

Goldstein, M. L., R. P. Lepping, and E. C. Sittler. “Magnetic Properties of Jupiter’s Tail at Distances from 80-7500 Jovian Radii,” September 1, 1984. https://ntrs.nasa.gov/citations/19860019428.

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This is a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

A detailed study of the magnetic field data from both Voyagers 1 and 2 has revealed several interesting properties of the near and distant Jovian magnetotail. During the first encounter, as Voyager 1 passed between 80 and 140 R sub J from Jupiter in the near tail, the spacecraft was almost entirely in the northerm lobe magnetic field. The frequency spectrum of magnetic fluctuation in this region cannot be characterized by a power law and does not appear to be turbulent. The distant tail spectra from Voyager 2 are compared with similar spectra obtained from Voyager 1 when it was in near radial alignment with Voyager 2. Although the gross properties of the tail and solar wind fields in most respects differ considerably, the shape and power levels of the spectra of the magnetic fluctuations are very similar, especially between .0001 and .001 Hz. At lower frequencies (.00001 to .0001 Hz) the spectra of magnetic helicity do differ.