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The spiral field inhibition of thermal conduction in two-fluid solar wind modelsThe paper reports on two-field models which include the inhibition of thermal conduction by the spiraling interplanetary field to determine whether any of the major conclusions obtained by Nerney and Barnes (1977) needs to be modified. Comparisons with straight field line models reveal that for most base conditions, the primary effect of the inhibition of thermal conduction is the bottling-up of heat in the electrons as well as the quite different temperature profiles at a large heliocentric radius. The spiral field solutions show that coronal hole boundary conditions do not correspond to states of high-speed streams as observed at 1 AU. The two-fluid models suggest that the spiral field inhibition of thermal conduction in the equatorial plane will generate higher gas pressures in comparison with flows along the solar rotation axis (between 1 and 10 AU). In particular, massive outflows of stellar winds, such as outflow from T Tauri stars, cannot be driven by thermal conduction. The conclusions of Nerney and Barnes remain essentially unchanged.
Document ID
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Nerney, S.
(NASA Ames Research Center Moffett Field, CA, United States)
Barnes, A.
(NASA Ames Research Center Space Sciences Div., Moffett Field, Calif., United States)
Date Acquired
August 9, 2013
Publication Date
August 1, 1978
Publication Information
Publication: Journal of Geophysical Research
Volume: 83
Subject Category
Solar Physics
Accession Number
Distribution Limits

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