An integrated Magneto-Fluid model, that accords full treatment to the Velocity fields associated with the directed plasma motion, is developed to investigate the dynamics of coronal structures. It is suggested that the interaction of the fluid and the magnetic aspects of plasma may be a crucial element in creating so much diversity in the solar atmosphere. It is shown that the structures which comprise the solar corona can be created by particle (plasma) flows observed near the Sun's surface -the primary heating of these structures is caused by the viscous dissipation of the flow kinetic energy.
Slit spectrograms of a quiescent prominence and the inner corona (h ~<2.5 arc min) in the range AA3400-7000 A (dispersion 6-10 A/mm) were obtained. From an analysis of the Stark effect on the Balmer lines (up to number 36) the electron density in the prominence n~ = (7 + 3) x 101~ cm -3 was deduced. The kinetic temperature Tk and the non-thermal velocities v~, found from a simultaneous consideration of the Balmer and metal lines, are T~ ~ 10 000 K and v~ ~ 6 km/s. Also the emission measure of the prominence along the line-of-sight was found: ME= 1031 cm -5.In the coronal spectrum 24 coronal lines were found. Thirteen of these lines were identified and measured photometrically to get their absolute intensities, profiles and halfwidths. For nine lines the intensities as a function of the height were studied and on this basis the coronal lines were divided into a few groups. The line-of-sight and non-thermal velocities are vT <~ 10 km/s and vt~ 25 km/s. The coronal lines originate in at least three types of regions with different temperatures. The emission measure as a function of the ionization temperature was determined. The abundances of four elements of the iron group (V, Cr, Mn, Co) were estimated. The abundances of the other elements of the same group (A, Ca, Fe, Ni), found from EUV-data, are in a good agreement with our observations. The degree of inhomogeneity in the corona was estimated: n~/(~,)2~ 3-10.
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