The calculation of theoretical chromospheric models and the interpretation of solar spectra from rockets and spacecraft

Details The calculation of theoretical chromospheric models and the interpretation of solar spectra from rockets and spacecraft The calculation of theoretical chromospheric models and the interpretation of solar spectra from rockets and spacecraft

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984sao..rept.....a&link_type=abstract

Semiannual Report, 1 Jan. - 31 Dec. 1983 Smithsonian Astrophysical Observatory, Cambridge, MA.

Astronomy and Astrophysics

Astrophysics

Chromosphere, Opacity, Solar Atmosphere, Sunspots, Ultraviolet Radiation, Atmospheric Models, Distribution Functions, Energy Levels, Hartree Approximation, Line Spectra, Prediction Analysis Techniques

Scientific paper

Models and spectra of sunspots were studied, because they are important to energy balance and variability discussions. Sunspot observations in the ultraviolet region 140 to 168 nn was obtained by the NRL High Resolution Telescope and Spectrograph. Extensive photometric observations of sunspot umbrae and prenumbrae in 10 chanels covering the wavelength region 387 to 3800 nm were made. Cool star opacities and model atmospheres were computed. The Sun is the first testcase, both to check the opacity calculations against the observed solar spectrum, and to check the purely theoretical model calculation against the observed solar energy distribution. Line lists were finally completed for all the molecules that are important in computing statistical opacities for energy balance and for radiative rate calculations in the Sun (except perhaps for sunspots). Because many of these bands are incompletely analyzed in the laboratory, the energy levels are not well enough known to predict wavelengths accurately for spectrum synthesis and for detailed comparison with the observations.

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