Physics
Scientific paper
Jan 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..755a&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 15, 1984, p. 755-760.
Physics
6
Cylindrical Plasmas, Magnetoplasmadynamics, Solar Corona, Solar Prominences, Coronal Loops, Magnetic Effects, Magnetohydrodynamic Stability, Plasma Equilibrium, Solar Magnetic Field, Solar Physics, Thermal Instability
Scientific paper
In order to understand the formation and stability of solar prominences, attention is given to the condensation modes of the thermal instability in a cylindriical plasma whose magnetic field has both potential (longitudinal) and nonpotential (poloidal) components forming helically twisted field lines. It is noted that the field line twist has a significant effect on the stability of condensation modes which are unstable if field lines are straight, but become stable as the twist increases. The problem is treated in a fully self-consistent way, to derive a second-order ordinary differential equation for radiative MHD stability. The approximation made by neglecting inertial terms is valid for coronal loop conditions if there is no singular surface in the plasma, and a simplified differential equation is derived. Attention is given to stability for the m = zero, 1, and 2 modes numerically, for various loop parameters.
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