The Solar Rotational Activity Variations during the 23-th Solar Cycle

Details The Solar Rotational Activity Variations during the 23-th Solar Cycle The Solar Rotational Activity Variations during the 23-th Solar Cycle

Mar 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006sunge...1a..39w&link_type=abstract

Sun and Geosphere, vol.1, no. 1, p. 39-42

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Scientific paper

The study of the solar activity variability has been of great interest since its discovery. On the one hand it is important for the understanding of the Sun as an active star and on the other hand for the investigations of the solar-terrestrial connections. The solar magnetic field reverses approximately every 22 years, and manifests the 11-year solar cycle, in which the Sun changes its activity from its maximum value to the minimum one. The activity variations, developed by the sun surface rotation in connection with the nonsymmetrical distribution of active regions over the solar disc appear in a shorter time scale. As it is well known, these variations have periods of about 27 days. The solar surface rotates with different velocity, depending on the latitude. The differential solar rotation period, observed from the Earth, varies from 26.75 days at the solar equator up to approximately 29 days at higher latitudes. However the observed periodicity is generally in a wider range: from 20 up to 36 days. This wider spread is a result of the combination of both active-region evolution and solar rotation. A simple empirical solar activity model is proposed, which describes the obtained behavior by harmonic oscillations with simultaneous amplitude and phase modulation. The solar rotational periodicity is analyzed using wavelet. It is demonstrated, that the model describes well the separate episodes of the active region evolution. Both kinds of modulations are the consequence of activity region growth or decay and hence, they are a result of a variable pattern of spots and active regions on the solar surface.

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