Formation of Be stars via wind accretion: Case study on Black hole + Be star binaries

TL;DR

This paper introduces a new formation scenario for black hole + Be star binaries via wind Roche lobe overflow, supported by simulations and population synthesis, predicting thousands of such systems in the Milky Way with wide, eccentric orbits.

Contribution

It presents the first detailed modeling of BH+Be binaries formed through WRLOF, estimating their population and orbital characteristics in the Milky Way.

Findings

Approximately 1800-3200 BHBe binaries in the Milky Way.

Systems have high eccentricities and wide orbits, with periods over 1000 days.

Potential for detection via astrometric and interferometric methods.

Abstract

Be stars are rapidly rotating main-sequence (MS) stars that play a crucial role in understanding stellar evolution and binary interactions. In this letter, we propose a new formation scenario for black hole (BH) + Be star binaries (hereafter BHBe binaries), where the Be star is produced through the Wind Roche Lobe Overflow (WRLOF) mechanism. Our analysis is based on numerical simulations of the WRLOF process in massive binaries, building upon recent theoretical work. We demonstrate that the WRLOF model can efficiently form BHBe binaries under reasonable assumptions on stellar wind velocities. Using rapid binary population synthesis, we estimate the population of such systems in the Milky Way, predicting approximately $\sim$ {1800-3200} currently existing BHBe binaries originating from the WRLOF channel. These systems are characterized by high eccentricities and exceptionally wide orbits, with typical orbital periods exceeding 1000 days and a peak distribution around $\sim$10000 days. Due to their long orbital separations, these BHBe binaries are promising targets for future detection via astrometric {and interferometric} observations.