Spectral investigation of new candidates to lambda Bootis type stars

I. V. Chernyshova; S. M. Andrievsky; W. W. Weiss; E. Paunzen; S.A. Korotin; Yu. V. Beletsky; U. Heiter; G. Handler; M. Weber

doi:10.1051/eas:2003027

All issues

Volume 6 (2003)

EAS Publications Series, 6 (2003) 271

Abstract

Issue		EAS Publications Series Volume 6, 2003 Observing with the VLTI


Page(s)		271 - 271
DOI		https://doi.org/10.1051/eas:2003027
Published online		31 January 2003

Observing with the VLTI
G. Perrin and F. Malbet (eds)
EAS Publications Series, 6 (2003) 271

Spectral investigation of new candidates to lambda Bootis type stars

I. V. Chernyshova¹, S. M. Andrievsky¹, W. W. Weiss², E. Paunzen², S.A. Korotin¹, Yu. V. Beletsky¹, U. Heiter³, G. Handler⁴ and M. Weber⁵

¹ Astronomical Observatory, Odessa National University, T.G. Shevchenko park, Odessa 65014, Ukraine;
² Institut für Astronomie der Universität Wien, Türkenschanzstr. 17, 1180 Wien, Austria
³ Department of Astronomy, Case Western Reserve University, 10900 Euclid Avenue, Cleveland, OH 44106-7215, USA
⁴ South African Astronomical Observatory, PO Box 9, Observatory 7935, South Africa
⁵ Astrophysical Institute Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany

Corresponding author: chern_irina@yahoo.com

Abstract

We made detailed abundance analysis for ultimative test of membership of twenty λ Bootis type stars candidates. Atmosphere parameters, LTE abundances for ten elements (including C and O) and NLTE values for Na were determined. We are able to confirm or establish the membership for nine objects (HD 23258, HD 36726, HD 40588, HD 74911, HD 84123, HD 91130, HD 106223, HD 111604 and HD 290799). Six stars (HD 90821, HD 98772, HD 103483, HD 108765, HD 201184 and HD 261904) can be definitely ruled out as being member of the λ Bootis group whereas no ambiguous decision can be drawn for another five stars (HD 66684, HD 105058, HD 120500, HD 141851 and HD 294253). We also tryed to find apparent spectroscopic binaries which have two solar abundant components mimic one metal-weak star as proposed by Faraggiana & Bonifacio (1999).