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

Kaiser, M. L. and Desch, M. D. and Brown, M. E. (1996) Evidence for an Io plasma torus influence on high-latitude Jovian radio emission. Journal of Geophysical Research A, 101 (A1). pp. 13-18. ISSN 0148-0227. http://resolver.caltech.edu/CaltechAUTHORS:20121002-103226694

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Abstract

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.


Item Type:Article
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http://dx.doi.org/10.1029/95JA02389DOIUNSPECIFIED
http://www.agu.org/pubs/crossref/1996/95JA02389.shtmlPublisherUNSPECIFIED
Additional Information:© 1996 American Geophysical Union. Received 1 May 1995; accepted 31 July 1995. The Editor thanks two referees for their assistance in evaluating this paper.
Record Number:CaltechAUTHORS:20121002-103226694
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20121002-103226694
Official Citation:Kaiser, M. L., M. D. Desch, and M. E. Brown (1996), Evidence for an Io plasma torus influence on high-latitude Jovian radio emission, J. Geophys. Res., 101(A1), 13–18, doi:10.1029/95JA02389.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:34620
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:02 Oct 2012 17:50
Last Modified:27 Dec 2012 02:47

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