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Magnetospheric convection at UranusThe unusual configuration of the Uranian magnetosphere leads to differences in the relative effects of solar wind induced magnetospheric convection and plasma corotation from those at the other planets. At the present epoch the orientation of the rotation axis of Uranus with respect to the solar wind flow direction leads to a decoupling of the convective and corotational flows, allowing plasma from the tail to move unimpeded through the inner magnetosphere. As Uranus progresses in its orbit around the sun, corotation plays a gradually more important role and the plasma residence times within the magnetosphere increase. When the rotation axis finally becomes perpendicular to the solar wind flow, corotation is dominant.
Document ID
19880063863
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Selesnick, R. S.
(MIT Cambridge, MA, United States)
Date Acquired
August 13, 2013
Publication Date
January 1, 1987
Subject Category
Lunar And Planetary Exploration
Accession Number
88A51090
Funding Number(s)
CONTRACT_GRANT: JPL-953733
Distribution Limits
Public
Copyright
Other

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