Journal
ASTROPHYSICAL JOURNAL
Volume 707, Issue 1, Pages 482-502Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/707/1/482
Keywords
solar-terrestrial relations; Sun: activity; Sun: atmosphere; Sun: chromosphere; Sun: faculae, plages; Sun: UV radiation
Categories
Funding
- NASA [NNX07AO75G, NAS5-97045]
- Air Force Office of Scientific Research (AFOSR) [FA9550-07-1-0565]
- DLR
- CNES
- ESA PRODEX program (Swiss contribution)
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Semiempirical atmospheric models of solar surface features as observed at moderate resolution are useful tools for understanding the observed solar spectral irradiance variations. Paper I described a set of models constructed to reproduce the observed radiance spectrum for solar surface features at similar to 2 arcsec resolution that constitute an average over small-scale features such as granulation. Paper II showed that a revision of previous models of low-chromospheric inter-network regions explains the observed infrared CO lines in addition to the UV and radio continuum from submillimeter to centimetric wavelengths. The present paper (1) shows that the Ca II H and K line wing observations are also explained by the new quiet-Sun-composite model, (2) introduces new low-chromospheric models of magnetic features that follow the ideas in Paper II, (3) introduces new upper chromospheric structures for all quiet-Sun and active-region models, and (4) shows how the new set of models explains EUV/FUV observations of spectral radiance and irradiance. This paper also discusses the chromospheric radiative-loss estimates in each of the magnetic features. The new set of models provides a basis for the spectral irradiance synthesis at EUV/FUV wavelengths based on the features observed on the solar surface.
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