Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh11a..05d&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH11A-05
Physics
7509 Corona, 7511 Coronal Holes
Scientific paper
A method for measuring the density, temperature, and velocity of coronal electrons was proposed by Reginald and Davila (2000) based on an extension the Thomson scattering theory of Cram (1976) to include flows. In this method the electron density is measured in the usual way (e.g. in LASCO or MkIV coronagraph images) by observing the total coronal intensity. The electron temperature and flow speed are obtained by obtaining ratios of spectral intensity measured in 50 A passbands or by fitting a portion of the spectrum to coronal models. Observations during the total solar eclipse of 2000 near Lusaka, Zambia demonstrated the feasibility of the method (Reginald et. al., 2003) using the first generation Multi-Aperture Coronal Spectrometer (MACS-1) instrument, and with the second-generation MACS in Libya in 2006 reasonable temperature and flow speeds were obtained. In this paper we continue this work by reporting on the results of new observations taken from the ground at the Solar-C coronagraph. Although eclipse measurements provide the best observation (nearly free of scattered light but with limited duration), the Solar-C coronagraph observations allowed several days of nearly continuous observation from which the repeatability and accuracy of the measurement could be determined. To deal with the increased atmospheric scatter, observations at Solar-C were done in polarized brightness (pB). Results will be reported in this talk.
Cyr Orville Chris St.
Davila Jose Manuel
Kuhn Jeff
Reginald N.
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