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Coronal density and temperature structure from coordinated observations associated with the total solar eclipse of 1988 March 18This paper explores and compares diagnostics for temperature and density within large-scale structures of the inner corona based on cospatial and cotemporal spectrophotometric observations made at the time of the total solar eclipse of 1988 March 17/18. In the analysis a determination of plasma temperature T can be derived unambiguously from the intensity ratios Fe XIV/XUV or Fe XIV/Fe X since all the emission lines come from the ionized state of Fe and the ratios are only weakly dependent on density. These temperatures and the densities found in well-defined large-scale coronal structures are discussed. The emission-line temperature is found to be high (local maxima) in the coronal structures with enhanced white-light emission and associated with new cycle high-latitude magnetic fields separated from the old cycle polar field of opposite polarity. Also the average of the ratio of scale-height temperature/temperature over the entire range of position angle is roughly unity although the ratio is higher than unity (1.3-1.6) in the three most prominent streamers.
Document ID
19920050412
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Guhathakurta, M.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Rottman, G. J.
(Colorado, University Boulder, United States)
Fisher, R. R.
(High Altitude Observatory Boulder, CO, United States)
Orrall, F. Q.
(Hawaii, University Honolulu, United States)
Altrock, R. C.
(National Solar Observatory; USAF, Phillips Laboratory, Sunspot NM, United States)
Date Acquired
August 15, 2013
Publication Date
April 1, 1992
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 388
ISSN: 0004-637X
Subject Category
Solar Physics
Accession Number
92A33036
Funding Number(s)
CONTRACT_GRANT: NAG5-633
Distribution Limits
Public
Copyright
Other

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