A dynamic relaxation technique for determining the structure and stability of coronal magnetic fields

Details A dynamic relaxation technique for determining the structure and stability of coronal magnetic fields A dynamic relaxation technique for determining the structure and stability of coronal magnetic fields

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...311..451c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 311, Dec. 1, 1986, p. 451-459.

Astronomy and Astrophysics

Astrophysics

39

Solar Corona, Solar Magnetic Field, Stellar Coronas, Stellar Magnetic Fields, Lorentz Force, Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamic Stability

Scientific paper

A new approach to the problem of determining the structure and stability of solar and stellar coronal magnetic fields is presented. It is pointed out that the conventional approach which proceeds by examining the linear stability of simple, analytic, but generally unrealistic equilibria fails to address many important questions - for example, the influence of finite-amplitude disturbances, the existence of multiple equilibria, or the possibility of perturbed boundary conditions. In contrast, the present paper invokes a Lagrange variable technique to formulate the problem dynamically as a mixed initial-value-boundary-value problem in three space dimensions. Thus, the determination of magnetic field structure is reduced to simulating the dynamic relaxation of an arbitrary initial magnetic field configuration toward equilibrium. The feasibility of the technique is illustrated by investigating straight but nonuniform twisted flux tubes as well as the typical 'twisted arch' topology of coronal loops.

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