Modeling 22-year solar activity cycle within framework of dynamo theory with allowance for primary field

Details Modeling 22-year solar activity cycle within framework of dynamo theory with allowance for primary field Modeling 22-year solar activity cycle within framework of dynamo theory with allowance for primary field

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985rpspr...4...14p&link_type=abstract

In its USSR Rept.: Space (JPRS-USP-85-003) p 14-15 (SEE N85-25284 15-12) Transl. into ENGLISH from Astronomicheskiy Zh. (USSR

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Dynamo Theory, Solar Activity, Solar Cycles, Solar Magnetic Field, Stellar Models, Magnetic Flux, Polarity, Sunspots

Scientific paper

The R. B. Leighton model was used in a description of evolution of the magnetic field on the Sun in the convective zone and at its surface. It was found that the maximum intensity which the background magnetic fields attain 2 years prior to the cycle maximum is 2.6 to 2.7 gauss in an epoch of an even cycle and 3.6 to 3.7 gauss in an epoch of an odd cycle at latitudes of about 10 to 20 deg N, S. The intensity of the polar fields averages 0.5 gauss, as is actually observed. A change in polarity of the polar fields occurs during the period of the solar activity maximum. Polar fields are formed by magnetic fields drifting from the middle latitudes. The middle-latitude fields have the polarity of the leading spots in the particular cycle and in each of the hemispheres. During the dropoff of the cycle the middle-latitude and equatorial fields have opposite polarity relative to the high-latitude fields. In the period of the minimum the magnetic fields in each of the hemispheres have an identical polarity. In the phase of growth of an odd cycle the middle- and high-latitude fields reverse their polarity. These and other findings reveal that the Leighton model gives a quite realistic distribution of background magnetic fields during two successive 11-year cycles.

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