Stokes V asymmetry and shift of spectral lines

Details Stokes V asymmetry and shift of spectral lines Stokes V asymmetry and shift of spectral lines

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...221..338g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 221, no. 2, Sept. 1989, p. 338-341.

Astronomy and Astrophysics

Astrophysics

61

Solar Atmosphere, Solar Magnetic Field, Solar Spectra, Spectral Line Width, Stokes Law Of Radiation, Asymmetry, Doppler Effect, Line Of Sight, Magnetic Flux, Zeeman Effect

Scientific paper

Further evidence is given for the interpretation of the observed unshifted and asymmetric Stokes V profiles in the solar atmosphere in terms of a magnetic flux concentration expanding with height and surrounded by a downflow. A general proof is given that a V profile originating in an atmosphere in which magnetic field and flow are spatially separated along the line of sight has a zero-crossing wavelength which is unshifted with respect to the rest wavelength of the line center. Heuristic considerations for the dependence of the asymmetry of Stokes V on Zeeman shift, Doppler shift, line width, and strength are described and confirmed by exploratory calculations.

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