Physics
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004kfnt...20..328l&link_type=abstract
Kinematika i Fizika Nebesnykh Tel, vol. 20, no. 4, p. 328-348
Physics
Scientific paper
The rotation of sector structures of large-scale magnetic fields of several types is studied from the analysis of the evolution of their main rotation period. For this purpose, we used the series of observations of solar background magnetic field (SBMF, 1904-2000) in the equatorial zone from +200) to -200 in latitude, of solar mean magnetic field (SMMF, 1975-2003), and of interplanetary magnetic field (IMF, 1947-2001). The rotation rate of the SBMF two-sector structure varied with about a 11-year cycle during the first half of the interval under investigation (around from 27 to 30 days) and with about a 8-year cycle during the second half (from 26.5 to 27.7 days). The four-sector structure had a 22-year cycle of rotation rate variability during the overall interval. The rotation synchronization of the main sector structures of SBMF took place during 1937-1957. We confirmed the existence of a rotation change of the Sun in the middle of the 20th century and revealed the change of the character of the SBMF sector structure, namely, the share of small-scale structures increased during the second half of the 20th century. The change of the IMP sector structure is observed which lies in the appearance of small-scale magnetic structures (the six-sector structure) during the last 20-30 years of the 20th century. The evolution of the main rotation periods of SBMF, SMMF, IMF is not identical during common intervals of observations. The rotation minimum period of the two-sector structure takes place during a low level of the solar activity in the case of SBMF and during a high level of the solar activity in the case of SMMF. The predominance of the four-sector structure of SMMF and IMF is observed during the same time intervals. Our results confirmed the idea that large-scale magnetic field is independent phenomenon of solar magnetism.
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