Magnetic field and turbulent velocities in the solar corona

A. B. Delone , G. A. Porfir'eva , O. B. Smirnova , and G. V. Yakunina
Sternberg State Astronomical Institute, Moscow, Russia


[1]  Observations conducted by the authors during total solar eclipses in 1968, 1981, and 1999 and the results of noneclipse observations in the visual, IR, and far UV regions of the solar spectrum obtained both on the ground and in the space (according to publications of other authors) are considered. The relation of nonthermal velocities to characteristics of the magnetic field is studied. The nonthermal velocities in coronal holes are found higher than in quiet corona. In quiet corona they are higher than in the coronal cavity around a quiet prominence. A conclusion is drawn that the difference in the turbulence in various structural formations in the corona is related to the magnetic field variability.

Received 16 November 2004; revised 29 March 2005; accepted 12 July 2005; published 18 October 2005.

Keywords: Coronal magnetic fields; Coronal turbulence; Coronal formations.

Index Terms: 7509 Solar Physics, Astrophysics, and Astronomy: Corona; 7511 Solar Physics, Astrophysics, and Astronomy: Coronal holes; 7524 Solar Physics, Astrophysics, and Astronomy: Magnetic fields.


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