Amplification of the Steady Toroidal Magnetic Field in Solar Interior and Asymmetry of Sunspot Activity in Neighbouring Cycles

Details Amplification of the Steady Toroidal Magnetic Field in Solar Interior and Asymmetry of Sunspot Activity in Neighbouring Cycles Amplification of the Steady Toroidal Magnetic Field in Solar Interior and Asymmetry of Sunspot Activity in Neighbouring Cycles

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...8e..19k&link_type=abstract

Solar and Stellar Activity Cycles, 26th meeting of the IAU, Joint Discussion 8, 17-18 August 2006, Prague, Czech Republic, JD08,

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Scientific paper

This investigation deals with the problem of the asymmetry of sunspot activity maximums in neighbouring solar cycles. The Gnevyshev-Ohl rule (Gnevyshev and Ohl 1948, Astron. Zhurn. 25, 18) is a likely evidence for the radiative interior pervaded by a strong steady magnetic field. Therefore, some effects are required to ensure existence this deep-laid field for long-duration times. The way for search of excitation mechanism of strong magnetic field gives us the helioseismological experiments. We take the physical parameters of the interiors from standard solar model by Allen (1973, Astrophysical Quantities, London) for calculations. It was found that main limiting factor on the magnetic field value is the magnetic flux loss due to buoyancy in the radiative (non-turbulent) zone (RZ) which overcomes the rate of the field decay caused by ohmic dissipation. The helioseismology inversions indicate that the radial, but not latitudinal, shear in the internal rotation of the Sun penetrates rather deep, almost to the solar core (Duval et al.1984, Nature 310, 22; Brown 1985, Nature 317, 591; Libbrecht 1986, Nature 319, 753). This radial differential rotation, acting on a weak relict poloidal magnetic field, about 1 G, in the stable RZ, can excite the rather strong steady toroidal fields (10 KG - 10 MG). Obtained estimations agree with the helioseismically determined magnetic intensities in the solar interiors (Dziembowski and Goode 1989, ApJ 347, 540; Antia, Chitre and Thompson 2003, A&A 399, 329). We assume that due to magnetic buoyancy and meridional circulation at the upper boundary of the RZ the power toroidal field may penetrate, partly, into the convective zone (CZ). Here stationary steady directed field will be add to oscillating toroidal field excited by αΩ-dynamo. Since the oscillating dynamo-field changes their own direction with 11-years cycle-period, then the amplitude of total, oscillating plus steady, toroidal field in the CZ has to be a few differing in neighbouring solar cycles. As a result, the sunspot activity ought to be not the same power too. This gives the opportunity to explain the asymmetry (alternation) of sunspot activity maximums in even and odd solar cycles.

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