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The impact of surface dynamo magnetic fields on the chemical abundance determination

Published online by Cambridge University Press:  24 July 2015

Nataliya G. Shchukina ,
Andrii V. Sukhorukov  and
Javier Trujillo Bueno
Nataliya G. Shchukina
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain email: natasha@iac.es Main Astronomical Observatory, National Academy of Sciences, 27 Zabolotnogo Street, Kiev 03680, Ukraine email: shchukin@mao.kiev.ua
Andrii V. Sukhorukov
Affiliation:
Main Astronomical Observatory, National Academy of Sciences, 27 Zabolotnogo Street, Kiev 03680, Ukraine email: shchukin@mao.kiev.ua Institute for Solar Physics, Department of Astronomy, Stockholm University, AlbaNova University Centre, SE-106 91, Stockholm, Sweden email: andrii.sukhorukov@astro.su.se
Javier Trujillo Bueno
Affiliation:
Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain email: natasha@iac.es Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain email: jtb@iac.es Consejo Superior de Investigaciones Científicas, Spain email: jtb@iac.es
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Abstract

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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.

Keywords

MHDdynamoline: formationradiative transferSun: abundancesSun
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Symposium S305: Polarimetry: From the Sun to Stars and Stellar Environments , December 2014 , pp. 368 - 371
Copyright
Copyright © International Astronomical Union 2015 

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