V643 Orionis: A detached, evolved, post-mass-exchange eclipsing binary⋆
The Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
2 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark
3 Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA 02138, USA
Accepted: 8 March 2019
Context. One of the greatest uncertainties in modelling the mass-exchange phases during the evolution of a binary system is the quantity of mass and angular momentum that has been lost from the system. To constrain this problem, a favourable, evolved, and detached real binary system is valuable as an example of the end result of this process.
Aims. We study the 52-day post-mass-exchange eclipsing binary V643 Ori from complete uvby light curves and high-resolution spectra. V643 Ori is double-lined and shows total primary eclipses. The orbit is accurately circular and the rotation of the two stars is synchronised with the orbit, but the photometry from a single year (1993) shows signs of weak spot activity (0.02 mag) around the primary eclipse.
Results. We determined accurate masses of 3.3 and 1.9 M⊙ from the spectroscopic orbit and solved the four light curves to determine radii of 16 and 21 R⊙, using the Wilson-Devinney photometric code. The rotational velocities from the cross-correlation profiles agree well with those computed from the known radii and orbital parameters. All observable parameters are thus very precisely determined, but the masses and radii of V643 Ori are incompatible with undisturbed post-main-sequence evolution.
Conclusions. We have attempted to simulate the past evolutionary history of V643 Ori under both conservative and non-conservative Case B mass transfer scenarios. In the non-conservative case we varied the amounts of mass and angular momentum loss needed to arrive at the present masses in a circular 52-day orbit, keeping the two stars detached and synchronised as now observed, but without following the evolution of other stellar properties in any detail. Multiple possible solutions were found. Further attempts were made using both the BSE formalism and the binary MESA code in order to track stellar evolution more closely, and make use of the measured radii and temperatures as important additional constraints. Those efforts yielded no satisfactory solutions, possibly due to limitations in handling mass transfer in evolved stars such as these. We remain hopeful that future theoreticians can more fully model the system under realistic conditions.
Key words: stars: evolution / stars: interiors / stars: rotation / binaries: eclipsing
Table 3 and the spectra (in FITS format) are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/624/A88
© ESO 2019