The origin and the diagnostic capabilities of the Stokes V asymmetry observed in solar faculae and the network

Details The origin and the diagnostic capabilities of the Stokes V asymmetry observed in solar faculae and the network The origin and the diagnostic capabilities of the Stokes V asymmetry observed in solar faculae and the network

Oct 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...224..225s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 224, no. 1-2, Oct. 1989, p. 225-241.

Astronomy and Astrophysics

Astrophysics

62

Faculae, Line Shape, Line Spectra, Magnetic Flux, Solar Magnetic Field, Photosphere, Solar Activity, Velocity Distribution

Scientific paper

The origin of the Stokes V asymmetry observed near disk center in solar active regions and in the quiet network is studied with the help of a two-dimensional flux tube model of solar magnetic elements. It is shown that the observed relative area and amplitude asymmetry, the zero-crossing wavelengths, and the width of four Fe I and II Stokes V profiles belonging to lines with widely different properties can be reproduced relatively well within the framework of the model incorporating certain features. The sensitivity of the Stokes V asymmetry to the thermal and velocity structure in and around solar magnetic elements is also demonstrated. It is the Stokes V line parameter most sensitive to the atmosphere in the vicinity of magnetic elements, and can also become a powerful diagnostic of the mass motions inside the magnetic elements. Values of the temperature and velocity in the immediate surroundings of these elements at the height of line formation are derived for the first time.

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