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Magnetic fields of low-mass main sequences stars: Nonlinear dynamo theory and mean-field numerical simulations. (arXiv:2308.08957v2 [astro-ph.SR] UPDATED)

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Our theoretical and numerical analysis have suggested that for low-mass main
sequences stars (of the spectral classes from M5 to G0) rotating much faster
than the Sun, the generated large-scale magnetic field is caused by the
mean-field $\alpha^2\Omega$ dynamo, whereby the $\alpha^2$ dynamo is modified
by a weak differential rotation. Even for a weak differential rotation, the
behaviour of the magnetic activity is changed drastically from aperiodic regime
to nonlinear oscillations and appearance of a chaotic behaviour with increase
of the differential rotation. Periods of the magnetic cycles decrease with
increase of the differential rotation, and they vary from tens to thousand
years. This long-term behaviour of the magnetic cycles may be related to the
characteristic time of the evolution of the magnetic helicity density of the
small-scale field. The performed analysis is based on the mean-field numerical
simulations of the $\alpha^2\Omega$ and $\alpha^2$ dynamos and a developed
nonlinear theory of $\alpha^2$ dynamo.

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