What is the difference between 'emission' and 'depression' contribution functions?

Details What is the difference between 'emission' and 'depression' contribution functions? What is the difference between 'emission' and 'depression' contribution functions?

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..136..239g&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 136, Dec. 1991, p. 239-250.

Physics

6

Absorption Spectra, Fraunhofer Lines, Photosphere, Solar Spectra, Emission Spectra, Line Spectra, Stellar Atmospheres

Scientific paper

The right approach to the problem of the depth of Fraunhofer line formation makes it possible to distinguish the main processes involved in the formation of a Fraunhofer line and to locate the depths for these processes in the photosphere. Physical and analytical (with the help of contribution functions) comprehension of these processes facilitates considerably the understanding of the notion of the depth of formation of Fraunhofer lines. This makes it possible to account for the connections of these processes with the origin and depth of location of different solar phenomena which are being investigated by using Fraunhofer lines.

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