Abstract
Significant coronal mass motions are deduced from soft X-ray line broadening observed in solar active regions even during quiescent periods. A large data base of Mg XI resonance line profiles near 9.17 A has been acquired with the SMM Flat Crystal Spectrometer for a variety of active region conditions and disk locations. For the X-ray bright areas, the typical profiles have an excess line width equal to or greater than the thermal Doppler width for Mg ions at the observed coronal temperatures (3-4 MK). The equivalent excess velocities of 40-60 km/s are higher than those reported previously for cooler lines in other wavebands. The excess velocities show a correlation with magnetic field strength or gradient, but no obvious dependence on the angular distance from sun center.
Published Version
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