Current-driven resistive ballooning modes in axially bounded solar flare plasmas

Details Current-driven resistive ballooning modes in axially bounded solar flare plasmas Current-driven resistive ballooning modes in axially bounded solar flare plasmas

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...325..468o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 325, Feb. 1, 1988, p. 468-475.

Astronomy and Astrophysics

Astrophysics

27

Coronal Loops, Current Sheets, Plasma Currents, Solar Flares, Computerized Simulation, Plasma Heating, Reynolds Number

Scientific paper

The most unstable current-driven resistive modes of an axially bounded coronal loop are found in computer simulations to exhibit the spatial structure of ballooning modes. The observed modes are not confined to mode rational surfaces, but instead have broad radial extent. A theory assuming ballooning mode spatial structure predicts that a minimum current should be required for linear instability, and that, when the mode is unstable, the linear growth rate scales linearly with the resistivity eta below a critical resistivity, and scales as cu root of eta for larger resistivities. Both predictions are borne out by simulation results. Both theory and simulation analyses of the mode suggest that the strong radial structure of the mode near the ends of the system is the primary contributing factor to the instability of the mode. A helical current sheet is formed in the nonlinear evolution of the mode near the edge of the current channel and is accompanied by a strong radial gradient in the current and partial current reversal.

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