Physics
Scientific paper
Apr 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...91..195v&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 91, April 1984, p. 195-217. Research supported by the Nederlandse Organisatie voor Zuiver-W
Physics
21
Solar Spectra, Solar Temperature, Sunspots, Umbras, Continuous Spectra, Line Spectra, Temperature Profiles
Scientific paper
From a high resolution spectrum of a sunspot umbra (1.1 to 2.3-micron wavelength), models of the temperature stratification in the deep layers of the umbra are derived. The observed spectrum is corrected for stray light using the H I Paschen line at 1.282-micron wavelength. A method is described for the iterative fitting of empirical temperature models to spectral information, and the method is applied to the present data. It is found that the observed profiles of three high-excitation lines of Si I and the observed continuum contrast between umbra and photosphere cannot be reproduced with a single, one-component model of the umbral atmosphere: the Si I lines require a model that is 460 K hotter at tau(0.5) = 3 than the continuum model. This indicates that hot and cool components coexist within the umbra. A temperature model derived from the relative intensity in the wings of three low-excitation lines of Mg I, Al I, and Si I is not significantly different from the continuum model.
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