Three-dimensional MHD simulation of the Parker instability in galactic gas disks and the solar atmosphere

Details Three-dimensional MHD simulation of the Parker instability in galactic gas disks and the solar atmosphere Three-dimensional MHD simulation of the Parker instability in galactic gas disks and the solar atmosphere

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasj...44..167m&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 44, no. 3, 1992, p. 167-175.

Astronomy and Astrophysics

Astronomy

37

Accretion Disks, Computerized Simulation, Galactic Structure, Magnetohydrodynamic Stability, Solar Atmosphere, Astronomical Models, Interstellar Matter

Scientific paper

3D magnetohydrodynamic simulations were performed in a study of the nonlinear evolution of the Parker instability in galactic gas disks and/or accretion disks, as well as in emerging flux regions (EFR) of the sun. The initial magnetic fields are parallel to one of the horizontal coordinates in magnetostatic equilibrium. The effect of coupling between the Parker (undular) instability and the interchange instability was studied. In both the galactic and solar cases, adjacent flux tubes move independently, so that a highly interleaved structure is created, although the expansion of magnetic loops induced by the Parker mode is similar to that found in 2D models. In galactic gas disks magnetic loops evacuate regions of interstellar space by accumulating interstellar gas in magnetic pockets. The accumulated gas is compressed by both infalling gas and horizontally expanding magnetic loops, forming dense, thin spurs. That is, the 3D nonlinear Parker instability creates a large-scale void-shell-spur structure, which is very similar to the large-scale structure of the universe as well as the interstellar gas and/or dust distribution. In the solar EFR model, magnetic loops expand into the corona, while the gas slides down along the magnetic field lines. An approximate self-similar expansion and shock wave formation at the loop footpoints (which were previously found in 2D loops) were observed in 3D loops. A horizontal expansion of the rising flux tubes produces vortex motions, which then generate torsional Alfven waves.

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