A comparison of solar proxy-magnetometry diagnostics

Details A comparison of solar proxy-magnetometry diagnostics A comparison of solar proxy-magnetometry diagnostics

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...452l..15l&link_type=abstract

Astronomy and Astrophysics, Volume 452, Issue 2, June III 2006, pp.L15-L18

Astronomy and Astrophysics

Astrophysics

13

Sun: Magnetic Fields, Sun: Granulation, Sun: Photosphere

Scientific paper

Aims.We test various proxy-magnetometry diagnostics, i.e., brightness signatures of small-scale magnetic elements, for studying magnetic field structures in the solar photosphere. Methods: .Images are numerically synthesized from a 3D solar magneto-convection simulation for, respectively, the G band at 430.5 nm, the CN band at 388.3 nm, and the blue wings of the H α, H β, Ca ii H, and Ca ii 854.2 nm lines. Results: .Both visual comparison and scatter diagrams of the computed intensity versus the magnetic field strength show that, in particular for somewhat spatially extended magnetic elements, the blue H α wing presents the best proxy-magnetometry diagnostic, followed by the blue wing of H β. The latter yields higher diffraction-limit resolution. Conclusions: .We recommend using the blue H α wing to locate and track small-scale photospheric magnetic elements through their brightness appearance.

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