A new technique for comparing solar dynamo models and observations

Autores
<div class="autor_fcen" id="5788">Mininni, P.D.</div>; <div class="autor_fcen" id="3802">Gómez, D.O.</div>
Año de publicación
2004
Idioma
inglés
Tipo de recurso
artículo
Estado
Versión publicada
Descripción
We present a new technique suitable for a detailed comparison between solar dynamo models and observations. The method is based on the technique of dynamo spectroscopy proposed by Hoyng & Schutgens (1995) and bi-orthogonal decomposition of solar data. This decomposition provides a representation of the mean and fluctuating components of the flows, yielding relevant information for the comparison. To illustrate the method, we use a simple kinematic dynamo model of the solar cycle. Irregularities are introduced in the evolution of the magnetic fields modeling the turbulent behavior of the solar convective region with a random perturbation on the external source for the poloidal field. After fine tuning the parameters of the model we obtain solar like solutions displaying a magnetic cycle of 22 years, with fluctuations in its period and amplitude. In addition, the model generates Maunder-like events with a time span of 60-100 years.
Fil:Mininni, P.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina.
Fuente
Astron. Astrophys. 2004;426(3):1065-1073
Materia
Magnetohydrodynamics (MHD)
Sun: magnetic fields
Sun: sunspots
Astrophysics
Chaos theory
Kinematics
Magnetic fields
Magnetohydrodynamics
Random processes
Satellite observatories
Spectroscopy
Solar cycle
Stochasticity
Sun: magnetic fields
Sun: sunspots
Sun
Nivel de accesibilidad
Acceso abierto
Licencia
http://creativecommons.org/licenses/by/2.5/ar
Repositorio
Biblioteca Digital (UBA-FCEN)
Institución
Universidad Nacional de Buenos Aires. Facultad de Ciencias Exactas y Naturales
OAI Identificador
snrd:HASH01a7ac5cce504d161d0fa72d