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A comparison of solar wind streams and coronal structure near solar minimumSolar wind data from the MIT detectors on the IMP 7 and 8 satellites and the SOLRAD 11B satellite for the solar-minimum period September-December, 1976, were compared with X-ray images of the solar corona taken by rocket-borne telescopes on September 16 and November 17, 1976. There was no compelling evidence that a coronal hole was the source of any high speed stream. Thus it is possible that either coronal holes were not the sources of all recurrent high-speed solar wind streams during the declining phase of the solar cycle, as might be inferred from the Skylab period, or there was a change in the appearance of some magnetic field regions near the time of solar minimum.
Document ID
19770059881
Document Type
Reprint (Version printed in journal)
Authors
Nolte, J. T. (American Science and Engineering, Inc. Cambridge, MA, United States)
Davis, J. M. (American Science and Engineering, Inc. Cambridge, MA, United States)
Gerassimenko, M. (American Science and Engineering, Inc. Cambridge, Mass., United States)
Lazarus, A. J. (American Science and Engineering, Inc. Cambridge, MA, United States)
Sullivan, J. D. (MIT Cambridge, Mass., United States)
Date Acquired
August 9, 2013
Publication Date
July 1, 1977
Publication Information
Publication: Geophysical Research Letters
Volume: 4
Subject Category
SOLAR PHYSICS
Funding Number(s)
CONTRACT_GRANT: NAS5-11062
CONTRACT_GRANT: F19628-75-C-0131
CONTRACT_GRANT: NAS2-8693
CONTRACT_GRANT: NAS8-27758
Distribution Limits
Public
Copyright
Other