Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...258..507s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 258, no. 2, p. 507-520.
Astronomy and Astrophysics
Astrophysics
19
Atmospheric Temperature, Chromosphere, Solar Activity Effects, Solar Atmosphere, Solar Magnetic Field, Spectroheliographs, Atmospheric Heating, Dwarf Stars, Flux Density, Line Spectra
Scientific paper
Spectroheliograms of quiet and active solar regions observed in spectral lines originating in the upper chromosphere and transition region are studied. Relationships between line intensities originating at different temperatures in the solar atmosphere are quantified presupposing a two-component model, comprising (1) a background basal emission and (2) a magnetically controlled emission which shows power-law dependences between emissions in different spectral lines. The spatial extent of coronal structures and substantial projection effects inhibit derivation of point-by-point intensity relationships for coronal emissions. The consistency of the results of the modeling yields strong evidence in favor of a basal emission component that is most likely nonmagnetic in origin. The basal component dominates the emission from outside the magnetic network, but is also present in pixels of at least moderate activity in network and plage, at a resolution of 5 x 5 arcsec. The inferred solar basal flux density in the C II (1335 A) line equals the basal flux found for solar-like dwarf stars. The distribution of intensities associated with the basal component is asymmetric, with a relatively strong high-intensity tail.
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