We investigated the generation of dynamo waves in the solar convection zone through a numerical simulation. We integrated the axisymmetric α– kinematic dynamo equations in a spherical geometry, where the α- and -profiles depend on the spatial coordinates. The model results show that the fundamental parameter that determines the behavior of the system is the product between the characteristic intensities of the α and contributions. In particular, we found three different regimes in which the system exhibits different behaviors: a regime without a dynamo effect, one with an exponential amplification of the magnetic field, and one with dynamo waves.
Kinematic Numerical Simulations of the Solar Dynamo: Dependence on alpha and omega values
Primavera L.;CARBONE, Vincenzo
2014-01-01
Abstract
We investigated the generation of dynamo waves in the solar convection zone through a numerical simulation. We integrated the axisymmetric α– kinematic dynamo equations in a spherical geometry, where the α- and -profiles depend on the spatial coordinates. The model results show that the fundamental parameter that determines the behavior of the system is the product between the characteristic intensities of the α and contributions. In particular, we found three different regimes in which the system exhibits different behaviors: a regime without a dynamo effect, one with an exponential amplification of the magnetic field, and one with dynamo waves.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
