Characteristics of magnetic solar-like cycles in a 3D MHD simulation of solar convection

• Autor(a) principal: Passos, D.
• Data de Publicação: 2014
• Outros Autores: Charbonneau, P.
• Tipo de documento: Artigo
• Idioma: eng
• Título da fonte: Repositório Científico de Acesso Aberto de Portugal (Repositórios Cientìficos)
• Texto Completo: http://hdl.handle.net/10400.1/11157
• topic: Spherical eedge geometry; Dynamo; Propagation; Models

We analyse the statistical properties of the stable magnetic cycle unfolding in an extended 3D magnetohydroclynamic simulation of solar convection produced with the EULAG-MHD code. The millennium,simulation spans over 1650 years, in the course of which forty polarity reversals take place on a regular similar to 40yr cadence, remaining well-synchronized across solar hemispheres. In order to characterize this cycle and facilitate its comparison with measures typically used to represent solar activity, we build two proxies for the magnetic field in the simulation mimicking the solar toroidal field and the polar radial field. Several quantities that characterize the cycle are measured (period, amplitudes, etc.) and correlations between them are computed, These are then compared with their observational analogs. From the typical Gnevyshesv-Ohl pattern, to hints of Gleissberg modulation the simulated cycles share many of the characteristics of their observational analogs even though the simulation lacks poloidal field regeneration through active region decay, a mechanism nowadays often considered an essential component of the solar dynamo. Some significant discrepancies are, also identified, most notably the in-phase variation of the simulated poloidal and toroidal large-scale magnetic components, and the low degree of hemispheric coupling at the level of hemispheric cycle amplitudes. Possible causes underlying these discrepancies are discussed.