Nonlinear Parker instability of isolated magnetic flux in a plasma

Details Nonlinear Parker instability of isolated magnetic flux in a plasma Nonlinear Parker instability of isolated magnetic flux in a plasma

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338..471s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 1, 1989, p. 471-492. Research supported by the U.S.-Japan Cooper

Astronomy and Astrophysics

Astrophysics

82

Chromosphere, Magnetic Flux, Magnetohydrodynamic Stability, Solar Atmosphere, Gravitational Effects, Magnetohydrodynamic Waves, Solar Corona, Velocity Distribution

Scientific paper

The nonlinear evolution of the Parker instability in an isolated horizontal magnetic-flux sheet embedded in a two-temperature layer atmosphere is studied by using a two-dimensional MHD code. In the solar case, this two-layer model is regarded as a simplified abstraction of the sun's photosphere/chromosphere and its overlying much hotter (coronal) envelope. The horizontal flux sheet is initially located in the lower temperature atmosphere so as to satisfy magnetostatic equilibrium under a constant gravitational acceleration. Ideal MHD is assumed, and only perturbations with k parallel to the magnetic-field lines are investigated. As the instability develops, the gas slides down the expanding loop, and the evacuated loop rises as a result of enhanced magnetic buoyancy. In the nonlinear regime of the instability, both the rise velocity of a magnetic loop and the local Alfven velocity at the top of the loop increase linearly with height and show self-similar behavior with height as long as the wavelength of the initial perturbation is much smaller than the horizontal size of the computing domain.

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