Physics
Scientific paper
Jun 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978soph...58...57p&link_type=abstract
Solar Physics, vol. 58, June 1978, p. 57-87.
Physics
58
Magnetohydrodynamic Stability, Solar Atmosphere, Solar Corona, Solar Magnetic Field, Solar X-Rays, Thermal Instability, Far Ultraviolet Radiation, H Alpha Line, Line Spectra, Solar Temperature, Taylor Instability
Scientific paper
The different types of coronal loop observed in EUV lines, H-alpha, and soft X-rays are reviewed. General physical considerations relevant to steady-state coronal magnetic loops are outlined. The possible role of thermal instability in loop development is discussed, the hydrostatic density variation along a loop of known temperature is estimated, and the magnetic-field variation along a loop is determined from the transverse force balance. Effects of twisting and magnetic-field concentration on loop structure are examined along with the importance of MHD instabilities. It is suggested that a lack of stable equilibrium at higher temperatures may be a cause of the cool loop cores recently observed in active-region loops, that an interchange mode on the lower side of a loop core is one of the most likely instabilities responsible for circulation of plasma in a loop, and that a hydromagnetic Rayleigh-Taylor instability may be important on the upper side of the core near the summit of an interconnecting loop whose core contains an enhanced magnetic field.
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