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Issue A&A
Volume 452, Number 2, June III 2006
Page(s) L15 - L18
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20065182



A&A 452, L15-L18 (2006)
DOI: 10.1051/0004-6361:20065182

Letter

A comparison of solar proxy-magnetometry diagnostics

J. Leenaarts1, R. J. Rutten1, 2, M. Carlsson2, 3 and H. Uitenbroek4

1  Sterrekundig Instituut, Postbus 80 000, 3508 TA Utrecht, The Netherlands
    e-mail: J.Leenaarts@astro.uu.nl
2  Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, Blindern, 0315 Oslo, Norway
3  Center of Mathematics for Applications, University of Oslo, PO Box 1053, Blindern, 0316 Oslo, Norway
4  NSO/Sacramento Peak, PO Box 62, Sunspot, NM 88349-0062, USA

(Received 10 March 2006 / Accepted 26 April 2006)

Abstract
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 $\alpha$, H $\beta$, 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 $\alpha$ wing presents the best proxy-magnetometry diagnostic, followed by the blue wing of H $\beta$. The latter yields higher diffraction-limit resolution.
Conclusions.We recommend using the blue H $\alpha$ wing to locate and track small-scale photospheric magnetic elements through their brightness appearance.


Key words: Sun: magnetic fields -- Sun: granulation -- Sun: photosphere




© ESO 2006

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