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The quasi-rigid rotation of coronal magnetic fieldsSpherical harmonic analysis and numerical simulations are used to study the rotational properties of the coronal magnetic field under the assumption that it can be approximated by a current-free extension of the photospheric field. It is found that the rotation rate in the outer corona is determined, principally, by coronal filtering, the global averages of the photospheric rotation rate, and ongoing source eruptions. The present model is able to account for observationally inferred rotational properties. It is suggested that the coronal rotation rate accelerates gradually due to the equatorward migration of sunspots, and that the 27-day equatorial period is approached toward sunspot minimum as the decaying photospheric flux becomes localized near the equator.
Document ID
19880043416
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Wang, Y.-M.
(Hulburt (E. O.) Center for Space Research Washington, DC, United States)
Sheeley, N. R., Jr.
(Hulburt (E. O.) Center for Space Research Washington, DC, United States)
Nash, A. G.
(Hulburt (E. O.) Center for Space Research Washington, DC, United States)
Shampine, L. R.
(U.S. Navy, E. O. Hulburt Center for Space Research, Washington DC, United States)
Date Acquired
August 13, 2013
Publication Date
April 1, 1988
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 327
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
88A30643
Funding Number(s)
CONTRACT_GRANT: DPR-W-14429
Distribution Limits
Public
Copyright
Other

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