Observed coronal temperatures at 1.37 solar radii in the region of a helmet structure

Details Observed coronal temperatures at 1.37 solar radii in the region of a helmet structure Observed coronal temperatures at 1.37 solar radii in the region of a helmet structure

Feb 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...40..387l&link_type=abstract

Solar Physics, vol. 40, Feb. 1975, p. 387-396. AEC-NSF-sponsored research.

Physics

7

Astronomical Models, Fine Structure, Solar Corona, Solar Eclipses, Solar Temperature, Emission Spectra, High Resolution, Magnetic Field Configurations, Radial Velocity, Solar Magnetic Field, Solar Spectra, Solar Wind, Spectral Line Width, Stellar Structure, Temperature Profiles

Scientific paper

During the total solar eclipse, 1965 May 30, a 25 cm aperture f/8.0 telescope and Fabry-Perot interferometer were operated aboard the USAF-AEC aircraft. High resolution spectra of the Fe XIV emission line, 530.3 nm, were obtained. Deconvolved intensity vs wavelength profiles of the second order fringe overlay a helmet structure on the NM limb at out to 1.37 solar radii. The profiles yield coronal temperatures, absolute intensities and Doppler velocities in regions of apparently open magnetic field structure and within the closed field lines of the helmet. Together with white light intensities the observations are interpreted to provide temperatures and turbulent velocities in and around this coronal structure. Comparison is made with a model by Billings and Roberts. We suggest a model with radial flow (solar wind) velocities of about 60 km per sec satisfies the observations in the open field line region.

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