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

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.

Current Status and Developments of the Atomic Database on Rare-Earths at Mons University (DREAM)

“…The use of oscillator strengths compiled in the DREAM database also allowed to identify new lanthanide lines in many different high-resolution astrophysical spectra and to deduce reliable abundances of rare earth elements (sometimes up to several orders of magnitude higher than the solar values in the case of various chemically peculiar stars), see, e.g., [45][46][47][48][49][50][51][52][53][54][55][56]. To give just one noteworthy specific example, we will mention the recent multicolour photometric investigation of the eclipsing binary system HD 66051 [53] carried out using, among other data, the spectroscopic parameters of the second and third spectra of lanthanides taken from the DREAM database.…”

ELISa: A new tool for fast modelling of eclipsing binaries

“…The temperature inhomogeneities can be caused by magnetic activity, such as in the case of variables of an RS CVn type (Pribulla et al 2000(Pribulla et al , 2001Vaňko et al 2007). Additionally, variations in the local chemical composition of the stellar surface, such as in the case of chemically peculiar stars (Strassmeier et al 2017;Paunzen et al 2018), can lead to spot variability. In the case of magnetic field-driven spots, the disturbances in a local magnetic field of the star with a convective envelope is capable of generating local suppression of convection that transfer energy from deeper parts of the star towards the surface.…”

The enigmatic highly peculiar binary system HD 66051

“…Niemczura et al 2017and Paunzen et al (2018) analyzed high-resolution spectra and photometric time series allowing them to determine the atmospheric parameters, the preliminary chemical composition of both stars, and orbital parameters (P = 4.749218 d) of the system. The primary component was found to be a slowly rotating late B-type star with a highly peculiar composition reminiscent of the primary in the SB1 system HD 65949, which seems to be its closest analogue.…”