Thermal instability excited in a plasma in the presence of a magnetic field

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Magnetic Fields, Magnetohydrodynamic Stability, Solar Atmosphere, Thermal Instability, Chromosphere, Electron Energy, Optical Thickness, Radiative Transfer, Solar Oscillations

Scientific paper

Thermal instability due to radiative energy losses is studied in the approximation of a two-component completely magnetized plasma. It turns out that in the case of motions transverse to the magnetic field, Field's (1965) conclusions in the one-fluid approximation must be modified considerably. Thus, the excited motions are not necessarily potential: they are often mainly vortical. The range of parameters for which the magnetic field plays a destabilizing role is considerably wider than Field's criterion implies. Another difference is that the thermal instability can be not only exponential, but also oscillatory. In the case of the solar chromosphere, the periods of oscillatory modes can be in the vicinity of several minutes.

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