MHD Simulations of Coronal Plasma Driven by Boundary Flows.

Details MHD Simulations of Coronal Plasma Driven by Boundary Flows. MHD Simulations of Coronal Plasma Driven by Boundary Flows.

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh13b..04t&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH13B-04

Physics

0644 Numerical Methods, 7509 Corona, 7524 Magnetic Fields

Scientific paper

A large portion of theoretical work on describing the large scale plasma evolution in solar and laboratory plasmas relies on Taylor's theory of relaxation which predicts that a plasma configuration will relax to a constant α profile, i.e., a force-free state with a constant in space coefficient of proportionality between the magnetic field and current density J = α B. Observations, however, show that α in the active region is a complex function of space (e.g. Zhang et al., 2001). In particular, the spatial profile of α consists of adjacent patches of opposite sign. We present a numerical MHD model of the dynamics of the active region plasma under photospheric boundary flows which addresses questions associated with the spatial structure of α. The simulations reveal that the evolution proceeds through a formation of adjacent, nearly force-free regions with parallel and anti-parallel magnetic fields and current densities, i.e. with α of opposite signs. We present the details of the model, explain the structure of the obtained solutions and the reason for the formation of such configurations. The boundary conditions are modeled by imposing a velocity profile and deriving consistent conditions on the magnetic field from the MHD equations. In order to address the numerical difficulties associated with the stiffness of the resistive MHD equations we use new exponential propagation iterative (EPI) methods which allow accurate time integration with time steps exceeding the CFL restriction on explicit schemes.

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