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Astron. Astrophys. 357, 351-358 (2000)

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Strong Stokes V asymmetries of photospheric spectral lines: What can they tell us about the magnetic field structure?

U. Grossmann-Doerth 1, M. Schüssler 2, M. Sigwarth 3 and O. Steiner 1

1 Kiepenheuer-Institut für Sonnenphysik, Schöneckstrasse 6, 79104 Freiburg, Germany
2 Kiepenheuer-Institut für Sonnenphysik, since 1 January 2000: Max-Planck-Institut für Aeronomie, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau, Germany
3 National Solar Observatory/Sacramento Peak, P.O. Box 62, Sunspot, NM 88349-0062, USA

Received 20 September 1999 / Accepted 8 February 2000


In an attempt to identify the mechanism responsible for the extremely asymmetric Stokes V profiles which were recently observed we analyzed several simple atmospheric configurations with separated layers of mass flow and magnetic field. We found that under appropriate conditions the models are capable of producing the observed one-lobe profiles.

Key words: line: formation – line: profiles – polarization – radiative transfer – Sun: magnetic fields

Send offprint requests to: O. Steiner (steiner@kis.uni-freiburg.de)

This article contains no SIMBAD objects.


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© European Southern Observatory (ESO) 2000

Online publication: May 3, 2000