Evidence for an Io plasma torus influence on high‐latitude Jovian radio emission | Zendy

Kaiser M. L. | Zendy; Desch M. D. | Zendy; Brown M. E. | Zendy

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Evidence for an Io plasma torus influence on high‐latitude Jovian radio emission

Author(s) -

Kaiser M. L.,

Desch M. D.,

Brown M. E.

Publication year - 1996

Publication title -

journal of geophysical research: space physics

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 1.67

H-Index - 298

eISSN - 2156-2202

pISSN - 0148-0227

DOI - 10.1029/95ja02389

Subject(s) - jovian , physics , torus , rotation period , astronomy , jupiter (rocket family) , plasma , astrophysics , radio wave , radio astronomy , wavelength , emission spectrum , spectral line , stars , spacecraft , planet , optics , geometry , mathematics , quantum mechanics , saturn

We report the discovery with the Ulysses unified radio and plasma wave (URAP) instrument of features in the Jovian hectometer (HOM) wavelength radio emission spectrum which recur with a period about 2–4% longer than the Jovian System III rotation period. We conclude that the auroral HOM emissions are periodically blocked from “view” by regions in the torus of higher than average density and that these regions rotate more slowly than System III and persist for considerable intervals of time. We have reexamined the Voyager planetary radio astronomy (PRA) data taken during the flybys in 1979 and have found similar features in the HOM spectrum. Contemporaneous observations by Brown (1994) show an [SII] emission line enhancement in the Io plasma torus that rotates more slowly than System III by the same amount as the HOM feature.

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