Bibcode
Shchukina, N. G.; Sukhorukov, A. V.; Trujillo Bueno, J.
Bibliographical reference
Proceedings of the International Astronomical Union, Volume 305, pp. 368-371
Advertised on:
10
2015
Citations
3
Refereed citations
3
Description
The solar abundances of Fe and of the CNO elements play an important
role in addressing a number of important issues such as the formation,
structure, and evolution of the Sun and the solar system, the origin of
the chemical elements, and the evolution of stars and galaxies. Despite
the large number of papers published on this issue, debates about the
solar abundances of these elements continue. The aim of the present
investigation is to quantify the impact of photospheric magnetic fields
on the determination of the solar chemical abundances. To this end, we
used two 3D snapshot models of the quiet solar photosphere with a
different magnetization taken from recent magneto-convection simulations
with small-scale dynamo action. Using such 3D models we have carried out
spectral synthesis for a large set of Fei, Ci, Ni, and Oi lines, in
order to derive abundance corrections caused by the magnetic, Zeeman
broadening of the intensity profiles and the magnetically induced
changes of the photospheric temperature structure. We find that if the
magnetism of the quiet solar photosphere is mainly produced by a
small-scale dynamo, then its impact on the determination of the
abundances of iron, carbon, nitrogen and oxygen is negligible.
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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