# The detached, evolved post-mass-exchange binary V643 Orionis

## TL;DR

This study analyzes the evolved binary V643 Ori to understand mass transfer effects, providing precise stellar parameters and testing evolutionary models, but finds current simulations insufficient to fully explain its history.

## Contribution

It offers detailed measurements of V643 Ori's stellar properties and evaluates different mass transfer scenarios using advanced modeling tools, highlighting limitations in current theoretical approaches.

## Key findings

- Masses of 3.3 and 1.9 solar masses determined
- Radii of 16 and 21 solar radii measured
- Current models do not fully reproduce the system's evolution

## Abstract

Context: One of the greatest uncertainties in modelling the mass-exchange phases during the evolution of a binary system is the amount 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 a double-lined, circular orbit, synchronized binary showing total primary eclipses. Results: We determine accurate masses of 3.3 and 1.9 M(Sun) and radii of 16 and 21 R(Sun). The masses and radii 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 synchronized 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 did not yield 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.