Other
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..19g&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Other
Scientific paper
The torsional oscillations of sunspot umbrae has been investigated on the observations of the longitudinal magnetic and velocity fields in the photospheric line FeI λ5253 Å of seven single sunspots. We reconstructed all three components of both fields from their line-of-sight components. The period of the umbra oscillations were limited within the boundaries of 2.2 - 7.1 days. All components of both vectors (magnetic and velocity) had the same oscillation periods without regard to the sunspot and had their own specific amplitude and initial phase. The initial phases of oscillations were distributed over the interval 0 - 2π. The oscillation magnetic energy of the components exceeded their kinetic energy by a factor up to 1000 (if the plasma density is 10^-7 g cm^-3). The azimuthal velocity calculated from velocity fields was more than the azimuthal velocity measured from the photoheliograms. The phase of the velocity azimuthal component oscillation was ahead of the phases of all other components of both vectors. The period of oscillations increase with latitude of the sunspot. It means, that torsional oscillations of sunspots are connected with the solar rotation.
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