Detection of Chromospheric Magnetic Fields: A Forward Modeling Approach

Details Detection of Chromospheric Magnetic Fields: A Forward Modeling Approach Detection of Chromospheric Magnetic Fields: A Forward Modeling Approach

Apr 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aspc..437..439u&link_type=abstract

Solar Polarization 6. Proceedings of a conference held in Maui, Hawaii, USA on May 30 to June 4, 2010. Edited by J. R. Kuhn, D.

Astronomy and Astrophysics

Astronomy

2

Scientific paper

We show that circular and linear polarization resulting from the Zeeman effect in chromospheric spectral lines is generally expected to be small because these lines form at high temperatures and arise from light elements. To illustrate this point we solve two-dimensional non-LTE radiative transfer in the Ca II 854.21 nm and Na I D2 lines through a magnetostatic flux concentration model and calculate the expected polarization. Finally, we show that the vertical magnetic field on the axis of the concentration can be recovered by measuring the bisector separation of the left- and right-hand circularly polarized emergent profiles.

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