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Lower Bound for Electron Core Beta in the Solar Wind

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dc.contributor.author Gary, S. P. en_US
dc.contributor.author Newbury, J. A. en_US
dc.contributor.author Goldstein, B. E. en_US
dc.date.accessioned 2004-09-24T20:37:11Z
dc.date.available 2004-09-24T20:37:11Z
dc.date.issued 1998-03 en_US
dc.identifier.citation Journal of Geophysical Research en_US
dc.identifier.citation USA en_US
dc.identifier.clearanceno 98-0585 en_US
dc.identifier.uri http://hdl.handle.net/2014/19283
dc.description.abstract Solar wind electrons, especially under conditions of relatively low speed flow, often can be represented as two bi-Maxwellian components, a cooler more dense core (denoted by the subscript c) and a hotter more tenuous halo. en_US
dc.format.extent 1175827 bytes
dc.format.mimetype application/pdf
dc.language.iso en_US
dc.subject.other solar wind electrons electron core beta Ulysses en_US
dc.title Lower Bound for Electron Core Beta in the Solar Wind en_US


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