Self-similar magnetohydrodynamics. I - The gamma = 4/3 polytrope and the coronal transient

Details Self-similar magnetohydrodynamics. I - The gamma = 4/3 polytrope and the coronal transient Self-similar magnetohydrodynamics. I - The gamma = 4/3 polytrope and the coronal transient

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...254..796l&link_type=abstract

Astrophysical Journal, Part 1, vol. 254, Mar. 15, 1982, p. 796-805.

Astronomy and Astrophysics

Astronomy

74

Magnetohydrodynamics, Polytropic Processes, Solar Corona, Stellar Atmospheres, Coronal Loops, Gamma Ray Astronomy, Gravitational Effects, Hydrodynamic Equations, Magnetic Field Configurations, Solar Limb, Stellar Magnetic Fields, Transient Response

Scientific paper

The full set of ideal magnetohydrodynamic (MHD) equations for a gamma = 4/3 polytrope admits self-similar solutions which can be derived by analytic methods. An axisymmetric magnetic field in a stratified stellar atmosphere is assumed. The solutions admit a large variety of magnetic structures, including those in the form of loops, moving through the corona with large scale coherence and sharp small scale features. The Lagrangian velocity of an individual transient feature is found to accelerate or decelerate according to a positive or negative gain in momentum by the plasma in a self-similar distribution of the Lorentz force, the pressure gradient, and the gravitational force. In both cases, the net force decreases with time so that, at large radial distances, the motion becomes inertial. The physical implications are discussed, arguring in favor of the transient beginning as a fully nonlinear MHD motion that ejects both magnetic field and plasma out of the gravitational bond of the sun.

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