Magnetic Coupling Between the Solar Surface and Corona: Theory and Observations

Details Magnetic Coupling Between the Solar Surface and Corona: Theory and Observations Magnetic Coupling Between the Solar Surface and Corona: Theory and Observations

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..703..203r&link_type=abstract

PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP Conference Proceedings, Volume 703, pp. 203

Physics

1

Photosphere, Interplanetary Magnetic Fields

Scientific paper

Multi-wavelength observations taken simultaneously by several instruments on the Solar and Heliospheric Observatory (SOHO) and Transition Region and Coronal Explorer (TRACE) revealed a clear connection between the photospheric magnetic fields and the energetic events in the overlying atmosphere. We find that the EUV coronal emission above the photosphere dominated by single polarity magnetic elements is spongy in space and has coherent braid-like structures in time. Contrary to these long living structures, corona above the regions with mixed polarity magnetic elements is highly discrete and consists of sporadic microflares, supersonic jets and their combinations. We believe that in the unipolar magnetic regions the energy flow from the surface to corona is associated with the nonlinear collective phenomena in the ensemble of oscillating magnetic flux tubes. These phenomena lead to formation of hot coronal ``clouds'' that have the properties of energetically open turbulence with tendency to self-organization. Jets and microflares above the mixed polarity regions are associated with shock waves produced by reconnecting magnetic flux tubes in the photosphere and subsequent interaction of shocks which leads to hydrodynamic cumulation of energy, which leads to impulsive phenomena similar to shaped charges.

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