Quasistatic evolution of magnetostatic coronal structures

Details Quasistatic evolution of magnetostatic coronal structures Quasistatic evolution of magnetostatic coronal structures

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..269w&link_type=abstract

In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 269-273 (SEE N87-20871 13-92)

Physics

Current Sheets, Equilibrium Equations, Magnetostatic Fields, Solar Corona, Solar Flux Density, Solar Wind, Electric Current, Lorentz Force, Pressure Gradients, Solar Gravitation, Solar Physics

Scientific paper

Four separate but related studies of coronal magnetostatic equilibria under a variety of boundary conditions and distributions of coronal current are reviewed. Physically, all four studies assume an axisymmetric corona whose radial magnetic field at the coronal base is dipolar. Electric currents in the model coronas are assumed to flow in the azimuthal direction, giving rise to Lorentz forces that must be balanced by pressure gradients and gravity. Mathematically, such coronas are described by the equation of magnetostatic force balance and Ampere's law. Although highly idealized, the axisymmetric magnetostatic models described provide insights into the behavior of a variety of coronal structures. The models show how more realistic current sheet boundary conditions and coronal density variations may be modeled.

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