A magnetic model of the solar transition region

Details A magnetic model of the solar transition region A magnetic model of the solar transition region

May 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976rspta.281..339g&link_type=abstract

(Royal Society, Discussion on the Physics of the Solar Atmosphere, London, England, Jan. 14, 15, 1975.) Royal Society (London),

Physics

274

Atmospheric Models, Chromosphere, Magnetic Field Configurations, Solar Atmosphere, Solar Magnetic Field, Convective Flow, Emission Spectra, Heat Balance, Magnetic Flux, Magnetohydrodynamic Flow, Solar Granulation, Stellar Models, Two Dimensional Models

Scientific paper

A two-dimensional model of the chromosphere and corona has been constructed, based on the magnetic-flux concentrations which occur at the boundaries of the supergranule convection cells. The expansion of the magnetic flux is determined by the vertical extent of the convecting plasma. The distribution of atmospheric material is consistent both with observed spectral intensities and with energy-balance requirements. The model predicts a primary transition region which is confined to an area about 10 arcsec wide overlying the supergranule boundaries. A secondary transition region, which is much thinner, covers the cell centers. The predictions are fully consistent with recent ultraviolet observations.

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