Chemical tracers of a highly eccentric AGB-main sequence star binary
Abstract
Binary interactions have been proposed to explain a variety of circumstellar structures seen around evolved stars, including asymptotic giant branch (AGB) stars and planetary nebulae. Studies resolving the circumstellar envelopes of AGB stars have revealed spirals, discs and bipolar outflows, with shaping attributed to interactions with a companion. For the first time, we have used a combined chemical and dynamical analysis to reveal a highly eccentric and long-period orbit for W Aquilae, a binary system containing an AGB star and a main sequence companion. Our results are based on anisotropic SiN emission, the first detections of NS and SiC towards an S-type star, and density structures observed in the CO emission. These features are all interpreted as having formed during periastron interactions. Our astrochemistry-based method can yield stringent constraints on the orbital parameters of long-period binaries containing AGB stars, and will be applicable to other systems.
Cite
@article{arxiv.2407.16979,
title = {Chemical tracers of a highly eccentric AGB-main sequence star binary},
author = {T. Danilovich and J. Malfait and M. Van de Sande and M. Montargès and P. Kervella and F. De Ceuster and A. Coenegrachts and T. J. Millar and A. M. S. Richards and L. Decin and C. A. Gottlieb and C. Pinte and E. De Beck and D. J. Price and K. T. Wong and J. Bolte and K. M. Menten and A. Baudry and A. de Koter and S. Etoka and D. Gobrecht and M. Gray and F. Herpin and M. Jeste and E. Lagadec and S. Maes and I. McDonald and L. Marinho and H. S. P. Müller and B. Pimpanuwat and J. M. C. Plane and R. Sahai and S. H. J. Wallström and J. Yates and A. Zijlstra},
journal= {arXiv preprint arXiv:2407.16979},
year = {2024}
}
Comments
This version of the article has been accepted for publication, after peer review (when applicable) and is subject to Springer Nature's AM terms of use, but is not the Version of Record and does not reflect post-acceptance improvements, or any corrections. The Version of Record is available online at: https://doi.org/10.1038/s41550-023-02154-y