Non-Axisymmetric Magnetic Fields and Flip-Flops on the Sun and Cool Stars

Details Non-Axisymmetric Magnetic Fields and Flip-Flops on the Sun and Cool Stars Non-Axisymmetric Magnetic Fields and Flip-Flops on the Sun and Cool Stars

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..224..123b&link_type=abstract

Solar Physics, Volume 224, Issue 1-2, pp. 123-131

Physics

15

Scientific paper

The modulation of solar activity closely follows the solar rotation period suggesting the existence of long-lived active regions at preferred longitudes. For instance, two preferred active longitudes in both southern and northern hemispheres are found to be persistent at the century time scale. These regions migrate with differential rotation and periodically alternate their activity levels showing a flip-flop cycle. The pattern and behaviour of active longitudes on the Sun is similar to that on cool, rapidly rotating stars with outer convective envelopes. This suggests that the magnetic dynamo, including non-axisymmetric magnetic fields and flip-flop cycles, is also similar in these stars. This allows us to overview the phenomenon of stellar magnetic activity and to study it in detail on the Sun.

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