MHD stability of compressible coronal loops with radiative energy loss

Details MHD stability of compressible coronal loops with radiative energy loss MHD stability of compressible coronal loops with radiative energy loss

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..352a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 1, 1984, p. 352-356.

Physics

8

Coronal Loops, Magnetohydrodynamic Stability, Solar Physics, Cylindrical Plasmas, Energy Dissipation, Plasma Compression, Plasma Currents, Radiation Effects, Solar Magnetic Field

Scientific paper

The effect of radiative energy loss on the stability of compressible plasma in coronal loops is studied. By taking the limit as poloidal wavenumber m approaches infinity, stability conditions for local modes are derived. It was found that the radiation effect can trigger MHD instabilities of coronal loops which are in ideally marginally stable states. Compressibility is a stabilizing effect for ideal MHD local modes because the compression of magnetic field lines exerts a restoring force by increasing magnetic pressure. Compression of plasma induces two modes in a radiatively unstable plasma, magnetosonic and condensation modes. Compressibility affects the stability of ideally stable (or unstable) coronal plasmas through magnetosonic modes, which are a stabilizing (destabilizing) effect for ideally stable (unstable) plasmas. For coronal plasmas in ideally marginally stable states, condensation as well as magnetosonic modes can trigger MHD instability. Because of these two modes, the effect of radiation on compressible coronal plasmas is more destabilizing than it is on incompressible plasmas when the plasmas are in ideal MHD unstable or marginally stable states.

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