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Stokes diagnostics of magneto-convection. Profile shapes and asymmetries

Published online by Cambridge University Press:  14 March 2005

E.V. Khomenko ,
S. Shelyag ,
S.K. Solanki ,
A. Vögler  and
M. Schüssler
E.V. Khomenko
Affiliation:
Instituto de Astrofísica de Canarias, Tenerife, Spain Main Astronomical Observatory, Kyiv, Ukraine email:[email protected]
S. Shelyag
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany email:[email protected], [email protected], [email protected], [email protected]
S.K. Solanki
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany email:[email protected], [email protected], [email protected], [email protected]
A. Vögler
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany email:[email protected], [email protected], [email protected], [email protected]
M. Schüssler
Affiliation:
Max-Planck-Institut für Aeronomie, Katlenburg-Lindau, Germany email:[email protected], [email protected], [email protected], [email protected]
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Abstract

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We discuss the polarization signals produced in recent realistic 3D simulations of solar magnetoconvection. The Stokes profiles of the Fe I 6301.5, 6302.5, 15648 and 15652 $\mathrm{\AA}$ Zeeman-sensitive spectral lines are synthesised and smeared to simulate the image degradation caused by the Earth's atmosphere and finite telescope resolution. A Principal Component Analysis approach is applied to classify the profiles. We find that the classes of Stokes $V$ profiles as well as their amplitude and area asymmetries are very close to the observations in the network and inter-network regions.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 635 - 636
Copyright
© 2004 International Astronomical Union