Large-Scale Magnetic Field and Sunspot Cycles |
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| Authors: | Makarov VI Tlatov AG CALLEBaUT DK Obridko VN Shelting BD |
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| Institution: | (1) Pulkovo Astronomical Observatory, 196140, Saint Petersburg, Russia;(2) Physics Department, UIA, University of Antwerp, B-2610, Belgium;(3) Institute of Terrestrial Magnetism, Ionosphere, and Radio Propagation (IZMIRAN), 142092 Troitsk, Moscow Region, Russia |
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| Abstract: | Hα magnetic synoptic charts of the Sun are processed for 1915–1999 and the spherical harmonics are calculated. It is shown
that the polarity distribution of the magnetic field on Hα charts is similar to the polarity distribution of the Stanford
magnetic field observations during 1975–1999. The index of activity of the large-scale magnetic field A(t), representing the sum of the intensities of dipole and octupole components, is introduced. It is shown that the cycle of
the large-scale magnetic field of the Sun precedes on the average by 5.5 years the sunspot activity cycle, W(t). This means that the weak large-scale magnetic fields of the Sun do not result from decay and diffusion of strong fields
from active regions as it is supposed in all modern theories of the solar cycle. On the basis of the new data the intensity
of the current solar cycle 23 is predicted and some aspects of the theory of the solar cycle are discussed. |
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