Magnetic fields of many astrophysical objects are sustained by convection in their interior (e.g., in the solar convective zone or the Earth's molten outer core); this mechanism of magnetic field generation is known as convective dynamo. Many spatial and temporal scales are present in astrophysical magnetic fields. To split large-scale and small-scale dynamics in the convective dynamo problem, asymptotic methods are applied. The object of this study is the large-scale stability analysis of the dynamo sustained by thermal convection in the idealised setup - in a rotating horizontal plane layer ofelectrically conducting fluid, with free electrically conducting boundaries.Evolution of large-scale perturbations of the regimes will be investigated by solving the system of the governing amplitude equations. The amplitude equations constitute a system of partialdifferential equations that reduces in some instances to the system of the mean-field equations. Various phenomena affect large-scale perturbations of convective hydromagnetic (CHM) regimes: kinematic and magnetic alpha-effect, anisotropic combined eddy diffusivity and eddy advection. These effects, governed by amplitude equations for perturbations of a short-scale CHM regime, will also be quantified for a number ofsymmetric CHM attractors that have been simulated by the candidate.
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