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Published online by Cambridge University Press: 11 May 2010
The quasimagnetostrophic equations are derived as a fourth-order asymptotic approximation of the ideal MHD equations written in spherical coordinates. A regular perturbation method is applied by expanding the nine dimensionless variables as asymptotic series in the Rossby number (Ro = O(∈)). The order of magnitude of the ten nondimensional parameters describing the flow is estimated for suitably characterising the interaction of large-scale dynamic and magnetic features at the interface between the radiative interior and the convective zone in the Sun. The importance of interactions between different low frequency modes (magnetostrophic, gravity and Rossby waves) in determining the topology of Solar activity structures is discussed.
INTRODUCTION
Starting with the paper of Parker (1955), one of the main purposes of scientists working in Solar physics was directed towards the understanding of the mechanisms governing the generation and the maintenance of the magnetic field that plays a central role in the Solar activity process. Many characteristic features, for example the well-known ‘butterfly’ diagram, are well described by kinematic dynamo theories. Great efforts are now directed towards the derivation of dynamo models that could agree with recent helioseismological data, and there is accumulating evidence that the seat of the dynamo is in the overshoot layer at the base of the convection zone (see for example, De Luca & Gilman 1991).
However, even the most sophisticated theories based mainly on the magnetic field are not able to explain topological aspects of Solar activity structures like active longitudes.
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