Cyclic evolution and reversal of the solar magnetic field. I. The large-scale magnetic fields

Details Cyclic evolution and reversal of the solar magnetic field. I. The large-scale magnetic fields Cyclic evolution and reversal of the solar magnetic field. I. The large-scale magnetic fields

2003-10-20

arxiv.org/abs/astro-ph/0310539v1

Astronomy and Astrophysics

Astrophysics

15 pages, 8 figures

Scientific paper

On the base of the solar magnetic field measurements obtained in Stanford in 1976--2003 the properties of the cyclic evolution of the large-scale magnetic field are investigated. Some regularities are found in longitudinal and latitudinal evolution of the magnetic field in cycles 21, 22 and 23. The cyclic development of the large-scale magnetic field can be divided into two main phases. The phase I, which includes a period approximately from two years before and until three years after the maximum of the solar cycle, is studied in detail. It is found that before the reversal of the large-scale magnetic field the neutral line of the magnetic field in antipodal longitudinal intervals shifts from the equator to opposite directions in cycles 21 and 22, but not in cycle 23. During the sign reversal of the large-scale magnetic field in cycles 21 and 22 in the antipodal longitudinal intervals the magnetic field of opposite polarity is observed in all latitudes, thereby forming an equatorial dipole. After the magnetic field reversal a longitudinal oscillation of the magnetic neutral line with regard to the equator takes place, which has a period about 2 years and damps to the minimum of the 11-year cycle. The intervening longitudinal intervals of the large-scale magnetic field correspond to positions of the active longitudes of sunspot activity, thus indicating a close connection of the large-scale and the local magnetic fields. In evolution of the large-scale magnetic field a periodicity with period $1.23\pm0.16$ year is revealed, which is close to the period found by helioseismological methods in variations of the solar rotation near the tachocline.

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