Empirical models of solar magnetic elements: constraints imposed by MgI Stokes profiles.

Details Empirical models of solar magnetic elements: constraints imposed by MgI Stokes profiles. Empirical models of solar magnetic elements: constraints imposed by MgI Stokes profiles.

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...299..596b&link_type=abstract

Astronomy and Astrophysics, v.299, p.596

Astronomy and Astrophysics

Astrophysics

27

Sun: Magnetic Fields, Sun: Activity, Sun: Faculae

Scientific paper

Although the temperature structure of small-scale magnetic features in the lower and middle photosphere has been constrained quite well, there are still considerable uncertainties in the upper photospheric and lower chromospheric thermal structure. As a step towards an improvement of this situation we investigate, using a non-LTE analysis, the diagnostic capabilities of the Stokes I and V profiles of the Mg I b_2_ 517.3nm and the Mg I 457.1nm lines. We find that the V profile of the former line can constrain the magnetic element thermal and velocity structure near the temperature minimum, which goes beyond the capabilities of the commonly used Fe I and II lines. The λ457.1nm line, on the other hand, does not provide any additional information on its own. A comparison of synthetic profiles with plage and network Stokes I and V spectra confirms the findings of Bruls & Solanki (???) that the chromospheric temperature rise starts at a substantially lower height in magnetic elements than in the quiet Sun. Some of the ambiguities in previous empirical models of magnetic elements are also removed. We confirm that small-scale magnetic features are associated with larger line broadening velocities than the quiet Sun, particularly in the higher layers. Finally, the Mg I b_2_ line is revealed to be a direct diagnostic of the merging height of magnetic elements.

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