Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...462.1137o&link_type=abstract
Astronomy and Astrophysics, Volume 462, Issue 3, February II 2007, pp.1137-1145
Astronomy and Astrophysics
Astrophysics
14
Radiative Transfer, Magnetic Fields, Line: Formation, Polarization, Sun: Photosphere, Sun: Magnetic Fields
Scientific paper
Aims:We introduce analytical response functions and their main properties as an important diagnostic tool that help understand Stokes profile formation physics and the meaning of well-known behaviors of standard inversion codes of the radiative transfer equation often used to measure solar magnetic fields. Methods: A Milne-Eddington model atmosphere is used as an example where response functions are analytical. A sample spectral line has been chosen to show the main qualitative properties. Results: We show that analytic response functions readily provide explanations for various well-known behaviors of spectral lines, such as the sensitivity of visible lines to weak magnetic fields or the trade-offs often detected in inversion codes between the Milne-Eddington thermodynamic parameters. We also show that response functions are helpful in selecting sample wavelengths optimized for specific parameter diagnostics.
Appendix A is only available in electronic form at http://www.aanda.org
Del Toro Iniesta Jose Carlos
Orozco Suárez David
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