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Slow twists of solar magnetic flux tubes and the polar magnetic field of the sunThe solar wind model of Weber and Davis (1967) is generalized to compute the heliospheric magnetic field resulting from solar rotation or a steady axisymmetric twist including a geometrical expansion which is more rapid than spherical. The calculated increase in the ratio of the toroidal to poloidal field components with heliocentric radial distance r clarifies an expression derived recently by Jokipii and Kota (1989). Magnetic-field components transverse to r do not in general grow to dominate the radial component at large r. The analysis also yields expressions for the Poynting flux associated with the steady twists.
Document ID
19890062607
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Hollweg, Joseph V.
(New Hampshire Univ. Durham, NH, United States)
Lee, Martin A.
(New Hampshire, University Durham, United States)
Date Acquired
August 14, 2013
Publication Date
August 1, 1989
Publication Information
Publication: Geophysical Research Letters
Volume: 16
ISSN: 0094-8276
Subject Category
Solar Physics
Accession Number
89A49978
Funding Number(s)
CONTRACT_GRANT: JPL-955461
CONTRACT_GRANT: NAGW-76
CONTRACT_GRANT: NSG-7411
Distribution Limits
Public
Copyright
Other

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