Physics – Plasma Physics
Scientific paper
Sep 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.346...23h&link_type=abstract
In ESA, Study of the Solar-Terrestrial System p 23-29 (SEE N93-31674 12-90)
Physics
Plasma Physics
4
Chromosphere, Collisions, Dense Plasmas, Ionic Collisions, Ionospheres, Magnetohydrodynamic Waves, Momentum Transfer, Spicules, Ionization, Mathematical Models, Plasma Physics, Solar Magnetic Field, Solar Wind
Scientific paper
With regard to solar plasma dynamics, the following topics are discussed: similarities and differences in the ionosphere; transmission of shear stress through the chromosphere; and the support of cold and dense chromospheric matter inside the hot and dilute corona against gravity. The chromosphere and ionosphere have in common that they contain weakly ionized plasmas. There are other similarities, but also strong differences. A most important one lies in the ratio of neutral ion coupling time to the propagation time of an Alfven wave through the respective regions. In the ionosphere this ratio is large, in the chromosphere it is very small. This has the consequence that only AC Pedersen currents exist in the latter region. Their properties are derived and their role for chromospheric heating and lifting of cool and dense plasma out of the chromosphere into the corona, to form spicules, is discussed. At the lower edge of the chromosphere, the temperature minimum region, electron-neutral collisions dominate ohmic resistivity. The related magnetic diffusivity sets a lower limit to the tranverse scale of current filaments on the order of 50 km. Twisted flux tubes with I approximately equal to 109 A can, however, exist. They can store substantial energy, up to 6 x 1027 ergs, and current dissipation in chromosphere and below can give rise to visible brightening such as faculae and filigree.
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