Orbital parameters and evolutionary status of the highly peculiar binary system HD 66051

¹ Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, 611 37 Brno, Czech Republic
e-mail: epaunzen@physics.muni.cz
² Faculty of Science, P. J. Šafárik University, Park Angelinum 9, Košice 040 01, Slovak Republic
³ Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Rabiańska 8, 87-100 Toruń, Poland
⁴ Centro de Tecnología Disruptiva, Universidad de San Pablo Tucumán, San Pablo, Tucumán, Argentina
⁵ American Association of Variable Star Observers (AAVSO), 49 Bay State Rd, Cambridge, MA 02138, USA
⁶ Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V. (BAV), 12169 Berlin, Germany
⁷ Vereniging Voor Sterrenkunde (VVS), Brugge 8000, Belgium
⁸ Instytut Astronomiczny, Uniwersytet Wrocławski, Kopernika 11, 51-622 Wrocław, Poland
⁹ Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
¹⁰ Laboratório Nacional de Astrofísica LNA/MCTI, R. Estados Unidos, 154, Itajubá 37504-364, MG, Brazil

Received: 7 November 2017
Accepted: 15 February 2018

Abstract

Context. The spectroscopic binary system HD 66051 (V414 Pup) consists of a highly peculiar CP3 (HgMn) star and an A-type component. It also shows out-of-eclipse variability that is due to chemical spots. This combination allows the derivation of tight constraints for the testing of time-dependent diffusion models.

Aims. We aim at deriving astrophysical parameters, information on age, and an orbital solution of the system.

Methods. We analysed radial velocity and photometric data using two different methods to determine astrophysical parameters and the orbit of the system. Appropriate isochrones were used to derive the age of the system.

Results. The orbital solution and the estimates from the isochrones are in excellent agreement with the estimates from a prior spectroscopic study. The system is very close to the zero-age main sequence and younger than 120 Myr.

Conclusions. HD 66051 is a most important spectroscopic binary system that can be used to test the predictions of the diffusion theory explaining the peculiar surface abundances of CP3 stars.