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New results of the spectral observations of CP stars

Published online by Cambridge University Press:  23 April 2010

N. S. Polosukhina ,
A. V. Shavrina ,
N. A. Drake ,
D. O. Kudryavtsev  and
M. A. Smirnova
N. S. Polosukhina
Affiliation:
Crimean Astrophysical Observatory, Nauchnyi, Crimea, Ukraine – email: [email protected]
A. V. Shavrina
Affiliation:
Main Astronomical Observatory of NAS of Ukraine, Kyiv, Ukraine
N. A. Drake
Affiliation:
Sobolev Astronomical Institute, St. Petersburg State University, Russia
D. O. Kudryavtsev
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Russia
M. A. Smirnova
Affiliation:
Crimean Astrophysical Observatory, Nauchnyi, Crimea, Ukraine – email: [email protected]
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Abstract

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The lithium problem in Ap-CP stars has been, for a long time, a subject of debate. Individual characteristics of CP stars, such as high abundance of the rare-earth elements presence of magnetic fields, complicate structure of the surface distribution of chemical elements, rapid oscillations of some CP-stars, make the detection of the lithium lines and the determination of the lithium abundance, a difficult task. During the International Meeting in Slovakia in 1996, the lithium problem in Ap-CP stars was discussed. The results of the Li study carried out in CrAO Polosukhina (1973–1976), the works of Hack & Faraggiana (1963), Wallerstein & Hack (1964), Faraggiana et al. (1992–1996) formed the basis of the International project ‘Lithium in the cool CP-stars with magnetic fields’. The main goal of the project was, using systematical observations of Ap-CP stars with phase rotation in the spectral regions of the resonance doublet Li I 6708 Å and subordinate 6104 Å lithium lines with different telescopes, to create a database, which will permit to explain the physical origin of anomalous Li abundance in the atmospheres of these stars.

Keywords

Stars: magnetic fieldsabundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 351 - 354
Copyright
Copyright © International Astronomical Union 2010

References

Faraggiana, R. 1992–1996, Mem. S. A. I.Google Scholar
Goriely, 2007, A&A, 466, 619Google Scholar
Hack, M. & Faraggina, R. 1963, PASPGoogle Scholar
Khan, 2004, JQSRT, 88, N1-3, 71Google Scholar
Kochuknov, O., Hoppe, P., & Zinner, E. 2004, A&A., 424, 935Google Scholar
Malanushenko, V. et al. 1992, A&A., 259, 567Google Scholar
North, et al. 1998, A&A, 333, 644Google Scholar
Panchuk, & Klochkova, , 1999.Google Scholar
Piskunov, & Valenti, 2002, A&A., 385, 109Google Scholar
Polosukhina, N. 1973–1976, Izv. CrAOGoogle Scholar
Polosukhina, N. et al. 1999, A&A, 351, 283Google Scholar
Shavrina, A. V. et al. 2008, Astrophysics, Vol. 51, p. 517CrossRefGoogle Scholar
Shavrina, A. V. et al. 2006 in Physics of Magnetic Stars. Proceedings of the Int. Conf., p. 341Google Scholar
Shavrina, A. V. et al. 2004, in The A-Star Puzzle, IAU Symp., 224, p. 711CrossRefGoogle Scholar
Shavrina, A. V. et al. 2001 A&A, 372, 571Google Scholar
Tzymbal, V. 1996, ASP Conf. Ser., 108, 198Google Scholar
Wallerstein, G. and Hack, M. 1964, The Observatory, Vol. 84, p. 160Google Scholar