Sunspot Rotations Derived from Magnetic and Velocity Fields Observations

Details Sunspot Rotations Derived from Magnetic and Velocity Fields Observations Sunspot Rotations Derived from Magnetic and Velocity Fields Observations

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005soph..231...11g&link_type=abstract

Solar Physics, Volume 231, Issue 1-2, pp. 11-21

Physics

10

Scientific paper

The rotation of sunspot penumbrae has been investigated on the longitudinal magnetic and velocity fields, observed in the photospheric line Fe I λ5253 Å of five lone sunspots. We reconstructed the entire vectors of both fields from their line-of-sight components. All three components of both vectors revealed that the rotation of the sunspots was, in fact, a torsional oscillation. All components of each sunspot had the same rotational period. The penumbrae oscillation periods were distributed in the range from 3.4 days to 7.7 days. The phase of the velocity azimuthal component oscillation was ahead of the phases of all other components of both vectors. If the penumbra plasma density had been equal to the photospheric plasma density (10-7 g cm-3) then the oscillation magnetic energy of the components exceeded their kinetic energy approximately by a factor of 10 200. The obtained results led to the conclusion that these oscillations were constrained.

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