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Spectrum Analysis of the Binary Star 53 Aur with a CP3 Component

Published online by Cambridge University Press:  12 April 2016

Juraj Zverko ,
Ján Budaj ,
Milan Zboril  and
Jozef Žižňovský
Juraj Zverko
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Czech and Slovak Federal Republic
Ján Budaj
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Czech and Slovak Federal Republic
Milan Zboril
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Czech and Slovak Federal Republic
Jozef Žižňovský
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranská Lomnica, Czech and Slovak Federal Republic

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The CP-star 53 Aur (HD 47152, HR 2425) has been assigned in the literature different types of peculiarity. Bertaud (1959) classified it as A0p-EuCr, Cowley et al. (1969) as B9p-Eu(Cr?), Osawa (1965) as Hg and Zverko (1974) as Mn -type. MacAlister (1978) discovered its binary nature and Tokovinin (1986) first determined its orbit with a period of 13.7 y. Subsequent interferometric observations by Baize (1989) yielded new orbital elements with a period of 25.816 y, total mass of 5.8 M⊙ and magnitude difference of two B9 components 0.3 mag. Adelman (1982) performed spectrophotometry and fitted the Balmer jump with Teff=10 500 K, while the Paschen continuum with Teff=9 500 K, log g=4 in both cases. Palmer (1965) estimated the projected rotational velocity to 325 km s−1 from the width of the Ca II-K line, while Wolff and Preston (1975) obtained 33 km s−1 from the Mg II 448.1 nm line. In this work we analyze high-dispersion spectra obtained in two distant orbital phases, namely in 1975 and in 1992 to distinguish the components of the system.

Type
I. General Properties of CP Stars
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 161 - 164
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Adelman, S.J. 1982, Astr. Ap. Suppl., 49, 663 Google Scholar
Baize, P. 1989, Astr. Ap. Suppl., 81, 415 Google Scholar
Balega, Yu.Yu., Balega, I.I. 1985, Pisma v Astr. Zh., 11, 112 Google Scholar
Bertaud, C. 1959, J. Obs., 42, 454 Google Scholar
Cowley, A.P., Cowley, C.R., Jaschek, M., Jaschek, C. 1969, Astr. J., 74, 375 Google Scholar
Hill, G. 1982, Pub. D.A.O., 16, 62 Google Scholar
Hubený, I. 1987, Scient, and Techn. Rep. Astr. Inst. Czechoslov. Acad. Sci., No. 40 Google Scholar
McAlister, H.A. 1978, Ap. J., 225, 932 CrossRefGoogle Scholar
Osawa, K. 1965, Ann. Tokyo Astr. Obs., 2nd Ser., 9, 123 Google Scholar
Palmer, D.R., Walker, E.N., Jones, D.H.P., Wallis, R.E. 1968, Royal Obs. Bull., No. 135, E 385 Google Scholar
Tokovinin, A.A. 1986, Pisma v Astr. Zh., 12, 480 Google Scholar
Wolff, S.C., Preston, G.W. 1978, Ap. J. Suppl., 37, 371 Google Scholar
Zverko, J. 1974, Bull. Astr. Inst. Czechoslov., 25, 321 Google Scholar
Zverko, J., Zboril, M., Žižňovský, J., Budaj, J.: 1992, In: Proceedings of the International Conference ”Stellar Magnetism”, ed. Glagolevski, Yu.V., in pressGoogle Scholar