Abstract Newly emerging magnetic flux can be the energy source for the solar corona and the solar wind. Plasma bulk motions and oscillations are observed by means of UV spectroscopy at transition zone (t.z.) temperatures (∼ 20.000 K < T < 250,000 K). The particular conditions in the transition zone plasma facilitate the conversion of magnetic into kinetic energy: (1) The β-value in the transition zone can change rapidly from β⪡1 to β⪢1. (2) Radiation losses change rapidly with temperature to create instabilities. (3) The small spatial filling factor (<0.01) indicates a highly filamented plasma. Large fluctuations in density, magnetic field strength and currents may facilitate fast reconnection. The areas of strong plasma oscillations in the transition zone may be the origin of coronal heating and particle acceleration.
Magnetic energy conversion in the solar transition zone
Advances in Space Research ; 10 , 9 ; 161-167
1990-01-01
7 pages
Article (Journal)
Electronic Resource
English
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