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Intensity of the Fe XV emission line corona, the level of geomagnetic activity, and the velocity of the solar windThe method of superposed epochs is used to determine the average solar wind velocity and the Kp index following central meridian passage of coronal weak and bright features identified from OSO 7 isophotograms of the Fe XV (284 A) emission line. It is found that bright coronal regions possess magnetic fields of closed configuration, thus reducing particle escape, while coronal holes possess open magnetic field lines favorable to particle escape or enhanced outflow of the solar wind.
Document ID
19760061663
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Bell, B.
(Harvard College Observatory and Smithsonian Astrophysical Observatory Cambridge, Mass., United States)
Noci, G.
(Harvard College Observatory and Smithsonian Astrophysical Observatory, Cambridge, Mass.; Arcetri, Osservatorio Astrofisico Florence, Italy)
Date Acquired
August 8, 2013
Publication Date
September 1, 1976
Publication Information
Publication: Journal of Geophysical Research
Volume: 81
Subject Category
Solar Physics
Accession Number
76A44629
Funding Number(s)
CONTRACT_GRANT: F19628-72-C-0146
CONTRACT_GRANT: NGR-22-007-211
CONTRACT_GRANT: F19628-75-C-0016
Distribution Limits
Public
Copyright
Other

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