Depths of the formation of magnetically sensitive absorption lines in the solar atmosphere

Details Depths of the formation of magnetically sensitive absorption lines in the solar atmosphere Depths of the formation of magnetically sensitive absorption lines in the solar atmosphere

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992kfnt....8...44s&link_type=abstract

Kinematika i Fizika Nebesnykh Tel (ISSN 0233-7665), vol. 8, no. 3, May-June 1992, p. 44-62. In Russian.

Computer Science

7

Absorption Spectra, Fraunhofer Lines, Polarized Radiation, Solar Atmosphere, Solar Magnetic Field, Photosphere, Spectral Line Width, Stokes Law Of Radiation

Scientific paper

The characteristics of the depression contribution functions for the Stokes profiles of the Fraunhofer lines formed in a magnetic field are investigated. The form of the depression functions depends mainly on the magnitude of the splitting and the Zeeman component intensity, and is of a complex nature with a pronounced asymmetry. These contribution functions are used to determine the depths of the formation of magnetically sensitive lines. The calculations show that, in a strong longitudinal magnetic field, the steep part of the line profile is formed higher than the center of the line profile. The Stokes profiles that describe the polarization characteristics are formed only several kilometers higher than the Stokes profile that specifies the general depression of the unpolarized and polarized radiation. The averaged depth of the formation of the whole line profile is virtually independent of the magnetic field strength. The depths of the formation of 17 photospheric lines usually used in magnetospectroscopic observations are calculated for models of the quiet photosphere, a flux tube, and the sunspot umbra.

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