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Line broadening of MG X 609 and 625 A coronal emission lines observed above the solar limb
Hassler, Donald M.; Rottman, Gary J.; Shoub, Edward C.; Holzer, Thomas E.
AA(Colorado, University, Boulder), AB(Colorado, University, Boulder), AC(High Altitude Observatory, Boulder, CO), AD(High Altitude Observatory, Boulder, CO)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 348, Jan. 10, 1990, p. L77-L80. (ApJL Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Line Shape, Magnetohydrodynamic Waves, Rocket Sounding, Solar Atmosphere, Solar Corona, Solar Limb, Emission Spectra, Line Spectra, Solar Spectra
Bibliographic Code:


A University of Colorado sounding rocket experiment on March 17, 1988, provided high-resolution EUV spectra along a solar diameter and out to 1.2 solar radius with spatial resolution of 20 x 60 arcsec. Each spectrum contains transition region and coronal emission lines in the wavelength range 605-635 A and 1210-1270 A, including the emission lines Mg X 609 and 625 A, Fe XII 1242 A, O V 629 A, N V 1238 and 1242 A, corresponding to a wide range of temperatures of formation. Increased line broadening is observed above the limb for all lines, and this effect is illustrated by presenting observed line widths as a function of height above the limb for the higher temperature lines Mg X 609 and 625 A. On the basis of calculations, the most likely cause of the increased broadening above the limb appears to be the presence of hydromagnetic waves in the corona.

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