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The evolution of a coronal streamer and the photospheric magnetic fieldA large equatorial coronal streamer observed in the outer corona grew in brightness and size during successive limb passages between October 6, 1973 and January 10, 1974 (solar rotations 1606-1611). Unlike previous studies of streamers and their photospheric associations, no definite surface feature could be identified in the present case. This suggests that the streamer is associated with the large scale photospheric magnetic field. Comparison of the streamer growth with observed underlying photospheric magnetic flux changes indicated that as the streamer increased in brightness, areal extent, and density, the photospheric magnetic flux decreased. Three possible explanations for the streamer's growth are presented, the conceptually simplest being that the decrease in photospheric field results in an opening of the flux tubes under the streamer, which permits an increase mass flux through the streamer.
Document ID
19810055442
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Poland, A. I.
(NASA Goddard Space Flight Center Greenbelt, MD; High Altitude Observatory, Boulder, CO, United States)
Macqueen, R. M.
(High Altitude Observatory Boulder, CO, United States)
Date Acquired
August 11, 2013
Publication Date
June 1, 1981
Publication Information
Publication: Solar Physics
Volume: 71
Subject Category
Solar Physics
Accession Number
81A39846
Funding Number(s)
CONTRACT_GRANT: NAS5-3950
Distribution Limits
Public
Copyright
Other

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