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The reversal of the solar polar magnetic fields. IV - The polar fields near sunspot maximumThe evolution of solar polar magnetic fields between Carrington rotations 1815 and 1834 is described using magnetic data from the Mount Wilson Observatory and the National Solar Observatory. The observations are compared with simulations using the flux transport equation. It is shown that the evolution of the polar field cannot be reproduced accurately by simulations of the diffusion and poleward drift of the emerging active regions at sunspot latitudes. Histograms of the distribution of the field intensities derived from daily magnetograms are presented which indicate that flux emerges at high latitudes and contributes to the evolution of the magnetic patterns.
Document ID
19930037313
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Murray, N.
(NASA Headquarters Washington, DC United States)
Wilson, P. R.
(California Inst. of Technology Pasadena, United States)
Date Acquired
August 16, 2013
Publication Date
December 1, 1992
Publication Information
Publication: Solar Physics
Volume: 142
Issue: 2
ISSN: 0038-0938
Subject Category
Solar Physics
Accession Number
93A21310
Funding Number(s)
CONTRACT_GRANT: N00014-89-J-1069
Distribution Limits
Public
Copyright
Other

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