Velocity fields associated with the magnetic component of solar faculae

Details Velocity fields associated with the magnetic component of solar faculae Velocity fields associated with the magnetic component of solar faculae

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.170...31s&link_type=abstract

(IAU, European Regional Astronomy Meeting, 11th, La Laguna, Spain, July 3-8, 1989) Astrophysics and Space Science (ISSN 0004-640

Astronomy and Astrophysics

Astrophysics

5

Faculae, Magnetic Field Configurations, Solar Magnetic Field, Velocity Distribution, Magnetic Flux, Optical Thickness, Solar Atmosphere

Scientific paper

Theoretical models are developed to account for the asymmetries observed by Stenflo et al. (1984) in the Stokes V profiles of solar faculae. The approximate dependence of Stokes V on magnetic and velocity fields in the line of sight is characterized under the assumption of local thermodynamic equilibrium, and empirical growth curves for the zero-crossing point of Stokes V are constructed. Good agreement between observed and theoretically predicted values is demonstrated for models in which there is no separation between magnetic layers and layers with velocity fields. The strength of the magnetic field increases toward the observer and the downflowing velocity field decreases, with the changes taking place in the same atmospheric layers.

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