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The analysis of Li i 6708A line through the rotational period of HD166473 taking into account Paschen-Back magnetic splitting

Published online by Cambridge University Press:  07 August 2014

A. V. Shavrina ,
V. Khalack ,
Y. Glagolevskij ,
D. Lyashko ,
J. Landstreet ,
F. Leone  and
M. Giarrusso
A. V. Shavrina
Affiliation:
Main Astronomical Observatory, Kyiv, Ukraine, email: shavrina@mao.kiev.ua
V. Khalack
Affiliation:
Université de Moncton, Moncton, N.-B., Canada, email: khalakv@umoncton.ca
Y. Glagolevskij
Affiliation:
Special Astrophysical Observatory, Nizhnij Arkhyz, Russia
D. Lyashko
Affiliation:
Tavrian National University, Simferopol, Ukraine
J. Landstreet
Affiliation:
University of Western Ontario, London, Canada Armagh Observatory, Armagh, Northern Ireland - United Kingdom
F. Leone
Affiliation:
Università di Catania, Catania, Italy
M. Giarrusso
Affiliation:
Università di Catania, Catania, Italy
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Abstract

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The analysis of Li i 6708 Å line was performed for 6 rotational phases distributed over the whole rotational period (~9.5 years) of HD166473. The magnetic field model was constructed based on the polarimetric measurements from Mathys et al. (2007). For each observed phase the modulus of the magnetic field was also estimated from simulation of the Fe ii 6147 Å, 6149 Å and Pr iii 6706.7 Å line profiles taking into account Zeeman magnetic splitting. The lithium abundance in each phase was obtained from fitting the observed Li i 6708 Å profile with the synthetic one calculated assuming Paschen-Back splitting and estimated magnetic field characteristics from Pr iii 6706.7 Å line profile.

Keywords

Stars: chemically peculiarstars: individual: HD166473
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 274 - 275
Copyright
Copyright © International Astronomical Union 2014 

References

Gelbmann, M., Ryabchikova, T., Weiss, W. W., Piskunov, N., Kupka, F., & Mathys, G. 2000, A&A, 356, 200Google Scholar
Gerth, E. & Glagolevskij, Y. 2003, Bulletin of SAO, 56, 25Google Scholar
Grevesse, N., Asplund, M., Sauval, A. J., & Scott, P. 2010, Ap&SS, 328, 179Google Scholar
Khalack, V. & Landstreet, J. 2012, MNRAS, 427, 569Google Scholar
Mathys, G., Kurtz, D. W., & Elkin, V. G. 2007, MNRAS, 380, 181CrossRefGoogle Scholar
Shavrina, A. V., Polosukhina, N. S., Khan, S., et al. 2006, Astron. Rep. 50 N6, 500Google Scholar
Shavrina, A. V., Polosukhina, N. S., Zverko, J., Khalack, V., Tsymbal, V. V. & Žižňovský, J. 2001, A&A, 372, 571Google Scholar
Stift, M. J., Leone, F. & Landi Degl'Innocenti, E. 2008, MNRAS 385, 1813Google Scholar