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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/283
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dc.contributor.authorLiebenberg, D. H-
dc.contributor.authorSanders, W. M-
dc.contributor.authorBrown, E. A-
dc.contributor.authorMurray, H. S-
dc.contributor.authorKennedy, R. N-
dc.date.accessioned2005-02-03T03:45:58Z-
dc.date.available2005-02-03T03:45:58Z-
dc.date.issued1980-06-
dc.identifier.citationBASI, Vol. 8, No. 2&3, pp. 49-57en
dc.identifier.urihttp://hdl.handle.net/2248/283-
dc.description.abstractWe have observed coronal emission line profiles at the February 16, 1980 total solar eclipse from an NC-135 aircraft. Very successful observations of a highly active corona near the peak of the 11 year solar cycle show considerable detail. The data from Fe XIV and Cz XV emission lines can be analysed to obtain detailed ion temperature and density with 4 arc-s spatial resolution and extending to beyond 2 solar radii in equatorial regions. Gradients of these parameters are related to coronal heating and solar wind acceleration processes. This paper describes the observations and methods of data analysis including the palnned comparisons with other available data from this time period.en
dc.format.extent1925946 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoen-
dc.publisherTata Institute of Fundamental Research, Bombayen
dc.subjectCoronal Emission Lineen
dc.subjectCoronal Emission Line Measurementen
dc.subjectTotal Solar Eclipseen
dc.titleCoronal Emission Line Measurements of the February 16, 1980 Total Solar Eclipseen
dc.typeArticleen
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