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Acceleration and heating of two-fluid solar wind by Alfven wavesEarlier model studies of solar wind driven by thermal pressure and Alfven waves have shown that wave amplitudes of 20-30 km/s at the coronal base are sufficient to accelerate the flow to the high speeds observed in quasi-steady streams emanating from large coronal holes. We focus on the energy balance in the proton gas and show that heat conduction from the region where the waves are dissipated may play an important role in determining the proton temperature at the orbit of Earth. In models with 'classical' heat conduction we find a correlation between high flow speed, high proton temperature, and low electron temperature at 1 AU. The effect of wave heating on the development of anisotropies in the solar wind proton gas pressure is also investigated in this study.
Document ID
19950033897
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Sandbaek, Ornulf
(Univ. of Oslo Blindern, Oslo, Norway)
Leer, Egil
(Univ. of Oslo Blindern, Oslo, Norway)
Date Acquired
August 16, 2013
Publication Date
March 1, 1994
Publication Information
Publication: The Astrophysical Journal, Part 1
Volume: 423
Issue: 1
ISSN: 0004-637X
Subject Category
Astrophysics
Accession Number
95A65496
Funding Number(s)
CONTRACT_GRANT: NASA ORDER W-17016
Distribution Limits
Public
Copyright
Other

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