Hostname: page-component-7bb8b95d7b-fmk2r Total loading time: 0 Render date: 2024-09-19T22:11:42.114Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopic Investigations of the Main-Sequence B Stars in the Association Cas OB2 and the Open Cluster Platais 1 (C2128+488)

Published online by Cambridge University Press:  12 April 2016

I.A. Usenko ,
V.V. Kovtjukh ,
S.M. Andrievsky ,
V.G. Klochkova ,
V.E. Panchuk  and
S.V. Ermakov
I.A. Usenko
Affiliation:
Department of Astronomy, Odessa State University, Shevchenko Park, 270014, Odessa, Ukraine
V.V. Kovtjukh
Affiliation:
Department of Astronomy, Odessa State University, Shevchenko Park, 270014, Odessa, Ukraine
S.M. Andrievsky
Affiliation:
Department of Astronomy, Odessa State University, Shevchenko Park, 270014, Odessa, Ukraine
V.G. Klochkova
Affiliation:
Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, 357147, Russia
V.E. Panchuk
Affiliation:
Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, 357147, Russia
S.V. Ermakov
Affiliation:
Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhnij Arkhyz, 357147, Russia

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A spectroscopic investigation of four main-sequence stars in the association Cas OB2 (HD 17327A and B, HD 16893, HD 17443) and of two stars in the open cluster Platais 1 (No. 1 (1921) and No. 111 (1600)) was carried out using high-resolution CCD spectra, obtained with echelle-spectrometer ”LYNX” (6-m telescope, Special Astrophysical Observatory, Russian Academy of Sciences). We have determined the atmospheric parameters for the program stars, their projected rotational velocities and elemental abundances in their atmospheres. Two new HgMn stars - HD 17327A and Platais No. 1 - were detected. HD 17443 is not a Be star.

Type
1. Overview
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 71 - 74
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Adelman, S.J., Philip, A.G.D., Adelman, C.J. 1996, MNRAS 282, 953 Google Scholar
Atutov, S.N., Shalagin, A.M., 1988, Soviet Ast.Lett. 14, 664 Google Scholar
Castelli, F., 1991, A&A 251, 106 Google Scholar
Galazutdinov, G.A. 1992, Prepr. SAO RAS No. 92Google Scholar
Hubeny, L., Lanz, T., Jeffrey, C.S. 1994, Newsletter Analys. Astron. Spec. No. 20, 30 Google Scholar
Kurucz, R.L. 1995, Laboratory and Astronomical High Resolution Spectra, Eds.Sauvai, A.J., Blomme, R., Grevesse, N., ASP Conf. Ser. 81, 595 Google Scholar
Kurucz, R.L. 1992, The Stellar Populations of Galaxies Eds. Barbuy, B., Renzini, A., IAU Symp. 149, 225 Google Scholar
Moon, T.T., Dworetsky, M.M., 1985, MNRAS 217, 305 Google Scholar
Panchuk, V.E., Najdenov, I.D., Klochkova, V.G., Ivanchik, A.B., Yermakov, S.V., Murzin, V.A. 1998, Bull. SAO RAS 44, 127 Google Scholar
Turner, D.G., Evans, N.R. 1984, ApJ 283, 254 Google Scholar
Turner, D.G., Mandushev, G.I., Forbes, D. 1994, AJ 107, 1796 Google Scholar