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A new determination of the solar rotation rateWe use 'stackplot' displays to compare observations of the photospheric magnetic field during sunspot cycle 21 with simulations based on the flux-transport model. Adopting nominal rates of diffusion, differential rotation, and meridional flow, we obtain slanted patterns similar to those of the observed field, even when the sources of flux are assigned random longitudes in the model. At low latitudes, the slopes of the nearly vertical patterns of simulated field are sensitive to the rotation rate used in the calculation, and insensitive to the rates of diffusion and flow during much of the sunspot cycle. Good agreement between the observed and simulated patterns requires a synodic equatorial rotation period of 26.75 +/- 0.05 days.
Document ID
19930035799
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Sheeley, N. R., Jr.
(NASA Headquarters Washington, DC United States)
Wang, Y.-M.
(NASA Headquarters Washington, DC United States)
Nash, A. G.
(U.S. Navy E.O. Hulburt Center for Space Research, Washington, United States)
Date Acquired
August 15, 2013
Publication Date
December 10, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 401
Issue: 1
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
93A19796
Funding Number(s)
CONTRACT_GRANT: NASA ORDER W-14429
Distribution Limits
Public
Copyright
Other

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