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J. M. Davila (NASA-GSFC), R. Nelson, O. C. St. Cyr (CUA)
Over the last 30-40 years spectroscopic observation of the EUV line emission has proved invaluable as a diagnostic of the solar coronal plasma state. Line ratios have been used to determine electron density, electron temperature and ion flow velocity. In this paper, we present results obtained with a new measurement technique that uses spectroscopic observations of the white light corona to obtain the electron density, temperature, and flow velocity.
A prototype instrument has been designed and built to obtain visible light spectra (3800-4300 A) with modest resolution. This instrument was used to obtain coronal observations during the June 2001 eclipse in Zambia. The data were corrected for sky and instrument transmission to derive the electron temperature and flow speed. Results from these measurements will be discussed.
The author(s) of this abstract have provided an email address for comments about the abstract: davila@linsay.gsfc.nasa.gov
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.