Scattering polarization in strong chromospheric lines. II. Influence of the temperature curve on the Ca II K line

Details Scattering polarization in strong chromospheric lines. II. Influence of the temperature curve on the Ca II K line Scattering polarization in strong chromospheric lines. II. Influence of the temperature curve on the Ca II K line

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...467..695h&link_type=abstract

Astronomy and Astrophysics, Volume 467, Issue 2, May IV 2007, pp.695-702

Astronomy and Astrophysics

Astrophysics

5

Line: Formation, Polarization, Radiative Transfer, Scattering, Sun: Atmosphere, Sun: Chromosphere

Scientific paper

In a previous paper we analyzed the polarization profile of the Ca II K line near the limb at μ = 0.1. We now extend this work to model the center-to-limb variation of the linear polarization of the Ca II K line and compare it with calculated spectra based on standard 1D model atmospheres. Our previous two-component approach with a hot and a cool atmospheric component is re-examined. We confirm our previous result that no single model is able to explain the observations. While self-consistent single atmosphere solutions may fit the polarization spectra, they fail to simultaneously fit the corresponding intensity spectra or the polarization spectra at other heliocentric angles. The mixing of a cool and a hot component is however a good approach for all disk positions, although the optimum mixing ratio varies strongly with heliocentric angle. As we approach the limb the hot component gains in importance, which is consistent with the scenario of diverging magnetic canopies overlying a cool atmosphere.

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