Population synthesis of Be X-ray binaries in the Small Magellanic Cloud: angular momentum recycling and stable mass transfer

TL;DR

This study uses binary population synthesis models to understand Be X-ray binaries in the Small Magellanic Cloud, focusing on mass transfer, angular momentum, and natal kicks, to match observed properties.

Contribution

It identifies the binary evolution parameters that best reproduce observed Be X-ray binaries, emphasizing stable Roche-lobe overflow and angular momentum recycling.

Findings

Models with stable Roche-lobe overflow and tidal angular momentum transfer best match observations.

Low natal kicks (less than 100 km/s) are favored by the models.

The propeller effect significantly influences the observable population and X-ray luminosity.

Abstract

Be X-ray binaries (BeXRBs) are key laboratories to constrain binary interaction processes such as mass transfer, angular-momentum transport, and natal kicks. The Small Magellanic Cloud (SMC), hosting a nearly complete and well-characterized BeXRB population, offers a unique opportunity to test these physical processes at low metallicity. We aim to identify the combination of binary-evolution parameters that simultaneously reproduces the observed number and the joint distribution of orbital period and optical magnitude of SMC BeXRBs. We performed an extensive grid analysis of binary population-synthesis models exploring different mass transfer efficiencies, angular-momentum transport prescriptions and Roche-lobe overflow stability criteria. We also considered the impact of natal kicks, and that of the propeller effect of rotating magnetic fields of neutron stars. Synthetic populations obtained with the binary population synthesis code \textsc{sevn} are statistically compared to observations using likelihood-based methods applied to the orbital period and $V$-band magnitude distributions, together with requirements on the total number of systems. We find that models in which mass transfer via Roche-lobe overflow is assumed to be always stable and angular momentum is recycled back into the orbit through tides when the accretor approaches critical rotation provide the best match to observations. Our best-fitting models favor low natal kicks ($\lesssim 100\ \rm km\ s^{-1}$), a moderate mass transfer efficiency ($f_{\rm MT} \simeq 0.6$), a minimum Be threshold spin close to critical rotation, and a strong suppression of accretion onto neutron stars due to the propeller effect. Specifically, the observable population is highly sensitive to the treatment of the propeller effect, which regulates the X-ray luminosity of wide, low-accretion-rate systems.