Background Magnetic Fields During Last 3 Cycles of Solar Activity

Details Background Magnetic Fields During Last 3 Cycles of Solar Activity Background Magnetic Fields During Last 3 Cycles of Solar Activity

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..30a&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

Physics

Scientific paper

The features of evolutions of magnetic fields of opposite signs and different intervals of the strength within ±100 Gs were studied. The research was based on observations carried out with the magnetograph for the longitudinal magnetic fields at the Kitt Peak Observatory during last 3 solar cycles. This material was kindly afforded by its authors. Next results were received: The solar magnetic field distribution is normal one with a maximum near 0 Gs. The half-width is equal 5 Gs. The imbalance of total magnetic fluxes within strength ± 100Gs during 3 cycles is equal ±0.36% of the sum of N- and S-polarity fluxes. Two groups of magnetic fields differing on the characteristics are allocated on the Sun. The magnetic fields of the first group have strength from 0 to ±100 Gs and are the most clearly seen within ±(3÷10) Gs. The magnetic fields of the second group appears when the strength becomes more then about ±(15÷20) Gs and are the most clearly seen when the strength is equal about ±(75÷100) Gs. The both types of fields are present in the interval ±(20÷100) Gs. The anomaly of the height of cycles obtained from total magnetic fluxes presents for 23d cycle in the second group of fields only.

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