Abstract
The photospheric magnetic data recorded from August 12, 1959 to September 29, 1967 and averaged over Bartels rotation periods are treated as zonal terms of the solar magnetic field which is expanded in a series of spherical harmonics. Numerical analysis of the reduced data gives seven periods. Three of these seem to be essential in the superposed variation of the solar magnetic field. The first of them (17.74 yr) is thought to be a contribution from the magnetic cycle for the determination of which the data covering only 8 yr interval are of insufficient accurity. For this reason, a 22.2 yr period is favoured by the computations. The numerical values of the two shorter periods are deduced as 2.557 yr and 4.194 yr. The amplitudes and phase angles of the periodic terms in question are determined.
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References
Csada, I. K.: 1959, Acta Phys. Chem. Szeged 5, 12.
Scherrer, P. H., Howard, R., and Wilcox, J.: 1971, in C. P. Sonett, P. J. Coleman Jr., and J. M. Wilcox (eds.), Solar Wind, NASA SP-308, p. 39; and 1972, Solar Phys. 22, 418.
Wilcox, J. M. and Ness, N. F.: 1965, J. Geophys. Res. 70, 5793.
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Csada, I.K. Short period variation of the photospheric magnetic field. Sol Phys 35, 325–330 (1974). https://doi.org/10.1007/BF00151954
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DOI: https://doi.org/10.1007/BF00151954