The prominence-corona interface: Models and observations

Details The prominence-corona interface: Models and observations The prominence-corona interface: Models and observations

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..177c&link_type=abstract

In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 177-1

Physics

Interfaces, Mathematical Models, Observation, Solar Corona, Solar Prominences, Astronomical Models, Chromosphere, Solar Magnetic Field, Solar Physics, Solar Radiation

Scientific paper

The Prominence Corona Interface (PCI) is discussed in the assumption that either: the threadlike structure observed in H alpha is due to density waves in an almost isothermal plasma and therefore, the PCI is present only around the bulk of the filament: the threadline structure is due to real cool threads imbedded in the hot coronal plasma and therefore, a PCI is present around each thread. In the latter case, the magnetic field is assumed parallel to the threads and the observed Differential Emission Measure (DEM) is very well reproduced by the assumption that the radiated energy is balanced by ohmic dissipation of Alfven waves at temperature T less than Tm and by the divergence of the conductive flux at T greater than Tm, where Tm is temperature of the minimum of DEM.

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