Metallicity dependence of Wolf-Rayet binaries using detailed binary models: An absence of long-period systems at low metallicity
Abstract
Observations of Wolf-Rayet (WR) stars in binaries in the SMC and LMC suggest a preference for short period (P≲30 days) orbits, with an apparent absence of WRs in long-period systems. The Galactic population does extend to longer periods but shows a deficit in long-period WR binaries compared to their progenitors, the O-star population. Across these populations a nearly constant binary fraction has been observed. We aim to characterize the population of WR binaries across a range of metallicity and determine the metallicity dependence of the formation of these systems, specifically focusing on the period distribution. We use detailed binary evolution models from POSYDON to predict the population of WR binaries at 0.01, 0.1, 0.2, 0.45, and 1Z⊙, analyzing the resulting period distribution and formation channels, while comparing them against the observed population in the SMC, LMC, and Milky Way. We find that the absence of wider WR binaries in the SMC, and potentially in the LMC, can be explained by stable, Case-B mass transfer only partially stripping the donor star, combined with WR winds at low metallicity being insufficiently strong to strip the remaining envelope. As a result, the long-period peak from Case-B mass transfer, present at Zsun, disappears at low metallicity. We additionally find that stable mass transfer (SMT) produces a short-period peak through Case-A mass transfer (P~5-10 days) that closely matches observations across metallicity. Furthermore, SMT and non-interacting systems are the dominant formation channels of WR binaries at all metallicities, with their relative contribution showing no metallicity dependence. This result implies that the SMT channel has the same metallicity-dependence as isolated WR formation. At the same time, we find that common envelope evolution primarily produces short-period (P<1 day) WR binaries with black-hole companions.
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BibTeX
@misc{briel2026metallicity,
title = {{Metallicity dependence of Wolf-Rayet binaries using detailed binary models: An absence of long-period systems at low metallicity}},
author = {Max M. Briel and Eirini Kasdagli and Tassos Fragos and Tomer Shenar and Jeff J. Andrews and Denzel Goh and Abhishek Chattaraj and Seth Gossage and Philipp Srivastava},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.05398},
eprint = {2609.05398},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.05398},
}
RIS
TY - UNPB
TI - Metallicity dependence of Wolf-Rayet binaries using detailed binary models: An absence of long-period systems at low metallicity
AU - Max M. Briel
AU - Eirini Kasdagli
AU - Tassos Fragos
AU - Tomer Shenar
AU - Jeff J. Andrews
AU - Denzel Goh
AU - Abhishek Chattaraj
AU - Seth Gossage
AU - Philipp Srivastava
PY - 2026
DA - 2026/09/04
PB - arXiv
DO - 10.48550/arxiv.2609.05398
UR - https://arxiv.org/abs/2609.05398
AB - Observations of Wolf-Rayet (WR) stars in binaries in the SMC and LMC suggest a preference for short period (P≲30 days) orbits, with an apparent absence of WRs in long-period systems. The Galactic population does extend to longer periods but shows a deficit in long-period WR binaries compared to their progenitors, the O-star population. Across these populations a nearly constant binary fraction has been observed. We aim to characterize the population of WR binaries across a range of metallicity and determine the metallicity dependence of the formation of these systems, specifically focusing on the period distribution. We use detailed binary evolution models from POSYDON to predict the population of WR binaries at 0.01, 0.1, 0.2, 0.45, and 1Z_⊙, analyzing the resulting period distribution and formation channels, while comparing them against the observed population in the SMC, LMC, and Milky Way. We find that the absence of wider WR binaries in the SMC, and potentially in the LMC, can be explained by stable, Case-B mass transfer only partially stripping the donor star, combined with WR winds at low metallicity being insufficiently strong to strip the remaining envelope. As a result, the long-period peak from Case-B mass transfer, present at Zsun, disappears at low metallicity. We additionally find that stable mass transfer (SMT) produces a short-period peak through Case-A mass transfer (P~5-10 days) that closely matches observations across metallicity. Furthermore, SMT and non-interacting systems are the dominant formation channels of WR binaries at all metallicities, with their relative contribution showing no metallicity dependence. This result implies that the SMT channel has the same metallicity-dependence as isolated WR formation. At the same time, we find that common envelope evolution primarily produces short-period (P<1 day) WR binaries with black-hole companions.
ER -