Magnetic field and nonthermal velocities in different coronal formations on the Sun

Details Magnetic field and nonthermal velocities in different coronal formations on the Sun Magnetic field and nonthermal velocities in different coronal formations on the Sun

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mast.conf..230y&link_type=abstract

Magnetic stars, Proceedings of the International Conference, held in the Special Astrophysical Observatory of the Russian AS, Au

Astronomy and Astrophysics

Astrophysics

Corona, Prominences, Magnetic Fields, Turbulence

Scientific paper

Profiles of coronal lines are used to investigate plasma movements in the solar corona. The nonthermal velocities ξ within coronal holes are higher and near quiet prominences they are smaller than in quiet coronal regions ranging from a dozen to several dozens km s-1 . Comparison of ξ-velocity magnitudes and magnetic field characteristics in different coronal formations allows us to believe that changes of turbulence in coronal plasma are caused by magnetic field variability. The authors' own observations during several eclipses and literature data have been used.

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