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Microstructures in the Polar Solar Wind: UlyssesWe find that small (10-200 rP) magnetic decreases comprise a dominant part of the polar solar wind microstructure at Ulysses distances (2.2 AU). These magnetic field dips are almost always bounded by tangential discontinuities, a feature which is not well understood at this time. Hundreds of these events have been examined in detail and a variety of types have been found. These will be described. It is speculated that these structures have been generated by perpendicular heating of ions closer to the Sun and have then been convected to distances of Ulysses. Such structures may be very important for the rapid cross- field diffusion of ions in the polar regions of the heliosphere.
Document ID
20000073293
Acquisition Source
Jet Propulsion Laboratory
Document Type
Other
Authors
Tsuruyani, Bruce T.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Arballo, J. K.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Galvan, C.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Goldstein, B. E.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Lakhina, G. S.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Sakurai, R.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Smith, E. J.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Neugebauer, M.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA United States)
Date Acquired
August 19, 2013
Publication Date
January 1, 1999
Subject Category
Solar Physics
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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