Dynamical plausibility of triple-assisted interaction in Be-star multiple systems
Abstract
Classical Be stars are rapidly rotating B-type stars surrounded by gaseous circumstellar disks, but the origin of their angular momentum remains uncertain. We investigate whether observed Be-star multiple systems are dynamically compatible with triple-assisted interaction, in which a tertiary companion drives Kozai-Lidov (KL) eccentricity excitation in an unresolved inner binary. We combine speckle-interferometric detections, reported inner periods, and proper-motion anomalies (PMa) with synthetic populations of hierarchical triples. Accepted configurations must satisfy dynamical stability, secular-timescale, inner-periastron interaction, and observational constraints. Refined mass-aware simulations identify HD 35079 and HD 55606 as the clearest period-plus-speckle dynamical matches. HD 205329 remains dynamically plausible but depends on the approximate PMa constraint. For HD 41335, the period-plus-speckle and PMa-plus-speckle constraints are separately compatible, whereas imposing all three simultaneously yields no accepted configurations at the adopted tolerance. HD 37330, HD 41600, and HD 71510 are additional PMa-dependent hierarchical-triple candidates. An independent angular-momentum estimate indicates a median required accreted mass fraction of approximately 4.8% under the adopted assumptions. We conclude that several observed Be-star multiple systems admit stable, KL-active architectures capable of driving inner binaries toward interaction. These results establish dynamical plausibility rather than a confirmed evolutionary history and motivate further speckle, spectroscopic, and astrometric monitoring.
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BibTeX
@misc{guerrero2026dynamical,
title = {{Dynamical plausibility of triple-assisted interaction in Be-star multiple systems}},
author = {C. A. Guerrero and O. V. Maryeva and M. Kraus},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.36304},
eprint = {2610.36304},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.36304},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Dynamical plausibility of triple-assisted interaction in Be-star multiple systems
AU - C. A. Guerrero
AU - O. V. Maryeva
AU - M. Kraus
PY - 2026
DA - 2026/10/26
PB - arXiv
DO - 10.48550/arxiv.2610.36304
UR - https://arxiv.org/abs/2610.36304
AB - Classical Be stars are rapidly rotating B-type stars surrounded by gaseous circumstellar disks, but the origin of their angular momentum remains uncertain. We investigate whether observed Be-star multiple systems are dynamically compatible with triple-assisted interaction, in which a tertiary companion drives Kozai-Lidov (KL) eccentricity excitation in an unresolved inner binary. We combine speckle-interferometric detections, reported inner periods, and proper-motion anomalies (PMa) with synthetic populations of hierarchical triples. Accepted configurations must satisfy dynamical stability, secular-timescale, inner-periastron interaction, and observational constraints. Refined mass-aware simulations identify HD 35079 and HD 55606 as the clearest period-plus-speckle dynamical matches. HD 205329 remains dynamically plausible but depends on the approximate PMa constraint. For HD 41335, the period-plus-speckle and PMa-plus-speckle constraints are separately compatible, whereas imposing all three simultaneously yields no accepted configurations at the adopted tolerance. HD 37330, HD 41600, and HD 71510 are additional PMa-dependent hierarchical-triple candidates. An independent angular-momentum estimate indicates a median required accreted mass fraction of approximately 4.8% under the adopted assumptions. We conclude that several observed Be-star multiple systems admit stable, KL-active architectures capable of driving inner binaries toward interaction. These results establish dynamical plausibility rather than a confirmed evolutionary history and motivate further speckle, spectroscopic, and astrometric monitoring.
ER -