Bibcode
Asensio Ramos, A.
Bibliographical reference
Astronomy and Astrophysics, Volume 563, id.A114, 9 pp.
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3
2014
Journal
Citations
3
Refereed citations
3
Description
A multiline Bayesian analysis of the Zeeman broadening in the solar
atmosphere is presented. A hierarchical probabilistic model, based on
the simple but realistic Milne-Eddington approximation to the solution
of the radiative transfer equation is used to explain the data in the
optical and near infrared. Our method makes use of the full line
profiles of more than 500 spectral lines from 4000 Å to 1.8 μm.
Although the problem suffers from a strong degeneracy between the
magnetic broadening and any other remaining broadening mechanism, the
hierarchical model allows the magnetic contribution to be isolated with
reliability. We obtain the cumulative distribution function for the
field strength and use it to put reliable upper limits on the unresolved
magnetic field strength in the solar atmosphere. The field is below
160-180 G with a 90% probability.
Related projects
Magnetism, Polarization and Radiative Transfer in Astrophysics
Magnetic fields pervade all astrophysical plasmas and govern most of the variability in the Universe at intermediate time scales. They are present in stars across the whole Hertzsprung-Russell diagram, in galaxies, and even perhaps in the intergalactic medium. Polarized light provides the most reliable source of information at our disposal for the
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