The optical depth of formation of weak Fraunhofer lines

Details The optical depth of formation of weak Fraunhofer lines The optical depth of formation of weak Fraunhofer lines

Apr 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981azh....58..403s&link_type=abstract

Astronomicheskii Zhurnal, vol. 58, Mar.-Apr. 1981, p. 403-407. In Russian.

Astronomy and Astrophysics

Astronomy

3

Fraunhofer Lines, Optical Thickness, Solar Atmosphere, Solar Spectra, Carbon Monoxide, Line Spectra, Rotational Spectra

Scientific paper

A relative-contribution function is proposed for determining the position and extent of the layer producing a weak Fraunhofer line for a given model of the solar atmosphere. As an example, the parameters of the layer in which lines of the first overtone of the vibration-rotation spectrum of CO are formed are calculated. It is found that the effective optical depth of formation of these lines increases with increasing excitation potential of the lower level; however, this shift does not exceed 80 K for lines with energies from 0.1 to 1.6 eV. At the limb the line is formed rather higher than at the center, but this shift only corresponds to a maximum of 100 K. Thus, various lines and various distances from the center exhibit practically the same CO layer, whose center of gravity is located in the optical depth range of 0.006 to 0.018, i.e., in the temperature range of 4660 + or - 75 K.

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