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Astron. Astrophys. 331, 639-650 (1998)

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The nearby ellipsoidal variable TV Pictoris *

K. Pavlovski 1, J. Cuypers 2, M. David 3, R.E.M. Griffin 4, H. Hensberge 2, S. Iliji 5, H. Schneider 6 and W. Verschueren ** 3

1 University of Zagreb, Faculty of Geodesy, Kaieva 26, 10000 Zagreb, Croatia
2 Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussel, Belgium
3 University of Antwerp (RUCA), Astrophysics Research Group, Groenenborgerlaan 171, B-2020 Antwerpen, Belgium
4 6 London Place, Oxford OX4 1BD, UK; currently visiting Department of Physics, University of Oxford, UK
5 Institute of Physics, Bijenika 34, 10000 Zagreb, Croatia
6 Universitäts-Sternwarte, Geismarlandstr. 11, D-37083 Göttingen, Germany

Received 27 June 1997 / Accepted 6 November 1997

Abstract

TV Pic is identified as a bright, near-contact mid-A + early-F binary seen under a moderate inclination of [FORMULA]. From the analyses reported in this paper, it appears that both components are undermassive (1.2 [FORMULA] 0.4 [FORMULA]), and that the secondary rotates not synchronously but more than twice as fast. These conclusions follow from the analysis of (1) high-dispersion spectra near both quadrature phases, to which the secondary contributes roughly 10% in the visual light, and (2) light-curves in the Strömgren and Walraven system covering the interval 3200-5600 Å and a time span of more than 2600 rotational periods. The light-curves show a very pronounced O'Connell effect, and only marginal colour variations. Models assuming a temperature spot either on the primary or the secondary explain the major part of the asymmetry in the light-curves, and are intended to provide useful initial estimates for more advanced mathematical codes. However, a more realistic physical model will require more discriminatory data, including spectroscopic observations in other spectral windows, and spectroscopy over the whole orbital cycle.

Key words: stars: binaries: close; spectroscopic – stars: individual: HD 30 861 (TV Pic) – stars: variables: other – stars: fundamental parameters – stars: rotation

* Based on observations obtained at the European Southern Observatory (ESO), La Silla, Chile
** Postdoctoral Fellow of the Fund for Scientific Research - Flanders (Belgium)

Send offprint requests to: K. Pavlovski (kresimir@geof.hr)

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© European Southern Observatory (ESO) 1998

Online publication: February 16, 1998
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