Rapid motion of filaments in active regions - Integral form of the equations of motion

Details Rapid motion of filaments in active regions - Integral form of the equations of motion Rapid motion of filaments in active regions - Integral form of the equations of motion

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989azh....66.1049m&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 66, Sept.-Oct. 1989, p. 1049-1060. In Russian.

Astronomy and Astrophysics

Astronomy

2

Chromosphere, Equations Of Motion, Integral Equations, Solar Activity, Solar Prominences, Differential Equations, Magnetohydrodynamics, Maxwell Equation, Solar Corona, Solar Magnetic Field

Scientific paper

The equations of motion of a filament are derived in integral form. Three components of the force are expressed in terms of surface integrals of the components of the Maxwell tensor at the level of the chromosphere. It is shown that, in the vicinity of the filament, the field transverse to it has an inversion region. This is a necessary condition for equilibrium of the current in an external field. On the surface of the chromosphere a line appears which is called the filament channel, the axis of a structure frequently observed in the chromosphere and having a palm-frond shape. As the filament ascends, this line is shifted into the weak-field region, which is related to the phenomenon of flare ribbon separation. The results apply to the current above the photosphere and provide a means of detecting (or measuring) it. This is the second such means, after measurement of the curvature of the unit vector of direction tau. An algorithm is proposed for determination of the magnetic field and Maxwellian tensor from the direction field tau in the problem of equilibrium and motion of a filament.

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