Volume 462, Number 3, February II 2007
|Page(s)||1137 - 1145|
|Published online||13 November 2006|
The usefulness of analytic response functions*
Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas, Apdo. de Correos 3004, 18080 Granada, Spain e-mail: firstname.lastname@example.org;email@example.com
Accepted: 8 October 2006
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.
Key words: radiative transfer / magnetic fields / line: formation / polarization / Sun: photosphere / Sun: magnetic fields
© ESO, 2007
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.