Ultra-high observations of the prominence-corona transition region

Details Ultra-high observations of the prominence-corona transition region Ultra-high observations of the prominence-corona transition region

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.344...49c&link_type=abstract

In ESA, Solar Physics and Astrophysics at Interferometric Resolution p 49-51 (SEE N93-10901 01-90)

Astronomy and Astrophysics

Astrophysics

High Resolution, Magnetohydrodynamic Waves, Plasma Layers, Solar Corona, Solar Prominences, Stellar Models, Mathematical Models, Solar Magnetic Field, Solar Wind

Scientific paper

Two models of the Prominence Corona Transition Region (PCTR) are analyzed in view of the possibility of ultrahigh resolution observations of UV lines on filaments and prominence. The first model assumes an isothermal cool filament (T less than 10,000 K) with a PCTR around it, while the second one assumes that a PCTR is present around each one of the thin H(alpha) threads which are usually observed in filaments. In this latter model, dissipation of Alfven waves is invoked to heat the power portion of the PCTR where the magnetic field is perpendicular (upside down Delta) T.

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