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On potential field models of the solar corona
Wang, Y.-M.; Sheeley, N. R., Jr.
AA(U.S. Navy, E.O. Hulburt Center for Space Research, Washington, DC), AB(U.S. Navy, E.O. Hulburt Center for Space Research, Washington, DC)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 392, no. 1, June 10, 1992, p. 310-319. Research supported by U.S. Navy. (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Magnetic Field Configurations, Solar Corona, Solar Magnetic Field, Coronal Holes, Iron, Magnetic Flux, Photosphere, Solar Atmosphere, Solar Spectra, Sunspots
Bibliographic Code:


It is shown that the line-of-sight matching procedure involved in potential field models of the solar corona do not make good use of the available data because there is strong evidence that the magnetic field is nearly radial, and therefore nonpotential, at the photosphere. It is argued that the observed photospheric field should first be corrected for line-of-sight projection and then matched to the radial component of the potential field. It is shown that this procedure yields much stronger polar fields than the standard method and produces better agreement with high-latitude coronal holes and with white-light structures in the outer corona. The relationship of both methods to the observed inclination angles of polar plumes is also discussed.

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