Microscopic filamentation due to electrothermal instability and plasma heating in time-dependent solar transition layer

Details Microscopic filamentation due to electrothermal instability and plasma heating in time-dependent solar transition layer Microscopic filamentation due to electrothermal instability and plasma heating in time-dependent solar transition layer

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988soph..116..239h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 116, no. 2, 1988, p. 239-258.

Physics

1

Magnetohydrodynamic Flow, Plasma Heating, Solar Heating, Solar Prominences, Atmospheric Heating, Plasma Currents, Solar Atmosphere, Solar Temperature

Scientific paper

The author has investigated nonlinear equilibrium states of a microscopic current filamentation (electrothermal instability) in solar atmosphere. The microscopic filamentation instability will develop for transition zone ion temperature plasmas, provided Te/Ti > 1, where Te and Ti are the electron and ion temperatures, respectively. When the onset condition for the electrothermal instability is satisfied, the instability drives a current filamentation to a nonlinear equilibrium state with a spatially periodic electron temperature variation with the wavelength comparable to several ion-Larmor radii. The amplitude of the periodic temperature variation may be so large that the transition layer temperature and coronal temperature plasmas may exist within several Larmor radii - coexistence of the transition zone and corona within the same macro-volume.

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