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The internal plasma state of the high speed solar wind at 1 AUThe character of particle velocity distributions in the high speed solar wind is described. It is found that electron distribution shapes differ from simple bi-Maxwellians in that a hot strongly beamed high energy electron component is always present, and is observed to move relative to a distinct low energy electron component along the magnetic field direction away from the sun. The velocity difference between hot and cold electron components appears, at times, to be strongly correlated with the local Alfven speed. Proton velocity distributions are also best represented by two relatively convecting unresolved components. Evidence is presented which supports the idea that the two-component proton structure observed in high speed regions is intimately related to fine scale velocity variations at 1 AU, and probably to prominent spatial and/or temporal structures present throughout that part of the corona from which the solar wind evolves.
Document ID
19770061372
Acquisition Source
Legacy CDMS
Document Type
Conference Proceedings
Authors
Feldman, W. C.
(Los Alamos Scientific Lab. NM, United States)
Abraham-Shrauner, B.
(Los Alamos Scientific Lab. NM, United States)
Asbridge, J. R.
(Los Alamos Scientific Lab. NM, United States)
Bame, S. J.
(California, University Los Alamos, N. Mex., United States)
Date Acquired
August 9, 2013
Publication Date
January 1, 1976
Subject Category
Solar Physics
Meeting Information
Meeting: International Symposium on Solar-Terrestrial Physics
Location: Boulder, CO
Start Date: June 7, 1976
End Date: June 18, 1976
Accession Number
77A44224
Distribution Limits
Public
Copyright
Other

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