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The Io plasma torus during the Cassi...

Steffl, Andrew Joseph.

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The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations.

Record Type:	Electronic resources : Monograph/item
Title/Author:	The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations./
Author:	Steffl, Andrew Joseph.
Description:	204 p.
Notes:	Source: Dissertation Abstracts International, Volume: 66-03, Section: B, page: 1512.
Contained By:	Dissertation Abstracts International66-03B.
Subject:	Physics, Astronomy and Astrophysics. -
Online resource:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3168299
ISBN:	0542044072

The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations.
Steffl, Andrew Joseph.

The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations. - 204 p.

Source: Dissertation Abstracts International, Volume: 66-03, Section: B, page: 1512.

Thesis (Ph.D.)--University of Colorado at Boulder, 2005.

During the Cassini spacecraft's flyby of Jupiter (1 October 2000 to 31 March 2001), the Ultraviolet Imaging Spectrograph (UVIS) produced an extensive dataset consisting of several thousand spectrally-dispersed images of the lo plasma torus. The temporal, radial, and azimuthal variability of the to plasma torus during this period are examined.

ISBN: 0542044072Subjects--Topical Terms:

1019521
Physics, Astronomy and Astrophysics.

The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations.
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020 $a 0542044072
035 $a (UnM)AAI3168299
035 $a AAI3168299
040 $a UnM $c UnM
100 1 $a Steffl, Andrew Joseph. $3 1905385
245 1 4 $a The Io plasma torus during the Cassini encounter with Jupiter: Temporal, radial and azimuthal variations.
300 $a 204 p.
500 $a Source: Dissertation Abstracts International, Volume: 66-03, Section: B, page: 1512.
500 $a Director: Fran Bagenal.
502 $a Thesis (Ph.D.)--University of Colorado at Boulder, 2005.
520 $a During the Cassini spacecraft's flyby of Jupiter (1 October 2000 to 31 March 2001), the Ultraviolet Imaging Spectrograph (UVIS) produced an extensive dataset consisting of several thousand spectrally-dispersed images of the lo plasma torus. The temporal, radial, and azimuthal variability of the to plasma torus during this period are examined.
520 $a The total EUV power radiated from the torus is found to be &sim;1.7 x 1012 W with variations of 25%. Several events were observed during which the torus brightened by 20% over a few hours. Significant changes in the composition of the torus plasma were observed between 1 October 2000 and 11 November 2000.
520 $a The composition and electron temperature of the torus plasma as a function of radial distance were derived from a scale of the midnight sector of the torus. The radial profile during the Cassini epoch shows significant differences from the Voyager era.
520 $a The Io torus is found to exhibit significant azimuthal variations in ion composition. This compositional variation is observed to have a period of 10.07 hours 1.5% longer than the System III rotation period of Jupiter. While exhibiting many similar characteristics, the periodicity in the UVIS data is 1.3% shorter than the "System IV" period. The amplitude of the azimuthal variation of S II and S IV varies between 5--25% during the observing period, while the amplitude of the variation of S III and O II remains in the range of 2--5%. The amplitude of the azimuthal compositional asymmetry appears to be modulated by its location in System III longitude.
520 $a The observed temporal variability is reproduced by models of the torus chemistry that include a factor of 3 increase in the rate of oxygen and sulfur atoms supplied to the extended neutral clouds that are the source of the torus plasma coupled with a &sim;35% increase in the amount of riot electrons in the Io torus. The observed azimuthal variability of the Io torus is well matched by models incorporating a primary source of hot electrons that slips 12.2°/day relative to the System III coordinate system and a secondary source of hot electrons that remains fixed in System III.
590 $a School code: 0051.
650 4 $a Physics, Astronomy and Astrophysics. $3 1019521
690 $a 0606
710 2 0 $a University of Colorado at Boulder. $3 1019435
773 0 $t Dissertation Abstracts International $g 66-03B.
790 1 0 $a Bagenal, Fran, $e advisor
790 $a 0051
791 $a Ph.D.
792 $a 2005
856 4 0 $u http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3168299