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Coronal Rotation at Solar Minimum from UV ObservationsUVCS/SOHO observations have been analyzed to reconstruct intensity time series of the O VI 1032 A and H 11216 A spectral lines at different coronal heliolatitudes from 1.5 to 3.0 solar radii from Sun center. Evidence was found for coronal differential rotation that differs significantly from that of the photospheric plasma. The study of the latitudinal variation shows that the UV corona decelerates toward the photospheric rates from the equator up to the poleward boundary 2 of the midlatitude streamers, reaching a peak of 28.16+/-0.20 days around +30 from the equator at 1.5 solar radii, while a less evident peak is observed in the northern hemisphere. This result suggests a real north-south rotational asymmetry as a consequence of different activity and weak coupling between the magnetic fields of the two hemispheres. The study of the radial rotation profiles shows that the corona is rotating almost rigidly with height.
Document ID
20090042322
Acquisition Source
Goddard Space Flight Center
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Mancuso, S.
Date Acquired
August 24, 2013
Publication Date
January 1, 2008
Publication Information
Publication: The Astrophysical Journal
Volume: 688
Subject Category
Solar Physics
Funding Number(s)
CONTRACT_GRANT: NNX08AQ96G
Distribution Limits
Public
Copyright
Other

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