A stringent upper limit on Be star fractions produced by binary interaction

TL;DR

This study establishes a rigorous upper limit on the fraction of Be stars formed through binary interactions, showing that binary evolution can account for up to one-third of Be stars in young clusters, aligning with observations.

Contribution

It provides a model-independent upper limit on Be star production via binary interaction and compares this limit with observations to evaluate binary evolution's role.

Findings

Binary interaction can produce at most one-third of Be stars in coeval populations.

Near the cluster turn-off, the upper limit matches observed Be star fractions.

Simple assumptions about unstable mass transfer fit observed Be fractions across masses.

Abstract

Context. Binary evolution can result in fast-rotating stars, predicted to be observable as Be stars, through accretion of angular momentum during mass-transfer phases. Despite numerous observational evidence pointing to this possibly being the dominant Be formation channel, current models struggle to produce a satisfactory description of Be star populations. Aims. Given distinct uncertainties in detailed binary evolution calculations, we investigate a rigorous and model independent upper limit for the production of Be stars through binary interaction and aim to confront this limit with observations of Be stars in young star clusters. Methods. Using extreme assumptions, we calculate the number ratio of post-interaction to pre-interaction binary systems in a coeval population, which describes an upper limit to Be star formation through mass-transfer. A detailed comparison is made between our derived upper limit and relevant observations of Be stars, which allows us to probe several aspects of binary star physics. Results. We find that in coeval populations, binary interaction can at most account for one third of all main-sequence stars being Be stars. Near the cluster turn-off region, this limit appears to be realised in the clusters studied. Away from the turn-off, applying simple assumptions about which systems undergo unstable mass-transfer produces a good fit to the observed Be fraction as a function of mass. Conclusions. We find that assuming distinct physics, binary evolution alone can in principle match the high numbers of Be stars observed in open clusters. Whether the required binary physics is realised in nature remains to be investigated.