Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989plap.work..189p&link_type=abstract
In ESA, Proceedings of an International School and Workshop on Plasma Astrophysics, Volume 1 p 189-195 (SEE N89-24910 18-75)
Astronomy and Astrophysics
Astrophysics
Magnetoplasmadynamics, Plasma Compression, Plasma-Electromagnetic Interaction, Solar Corona, Solar Flares, Solar Prominences, Magnetic Disturbances, Magnetic Field Reconnection, Solar Magnetic Field, Stellar Mass Ejection
Scientific paper
It is suggested that the highly structured nature of the solar corona can be understood in terms of standing MHD disturbances of several types, spread over extended regions. They can be compressions (fast or slow mode), in which the plasma pressure increases, or expansions (fast or slow mode) in which it decreases. Such interactions are also present in the inflow region of 2D steady-state magnetic reconnection models. Reconnection of 3D magnetic fields occurs when an electric field exists along a singular line (a field line with an X-type topology nearby). In general a sheared field possesses a continuum of potential singular lines and which one supports reconnection depends on the flow or electric field. Constraints on the electric field and flow are presented for reconnection at a given singular line. Such reconnection is accompanied by strong plasma jetting along the singular line. It is proposed that solar prominences are located in large curved flux tubes which are twisted up by Coriolis forces. When the twist is large enough the magnetic field near the summit has the required curvature to support plasma against gravity. As the twist increases the prominence grows in length and eventually loses equilibrium and erupts outwards into interplanetary space with a coronal mass ejection.
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