Binaries: close; Stars: individual: HD 98800; Stars: pre-main sequence; Techniques: high angular resolution; Techniques: interferometric; Orbital parameters; Orbitals; Quadruple systems; Radial velocity; Star: individual: HD 98800; Stars: individual: proxima Centauri; Technique: interferometric; Techniques: high angular resolutions; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.SR; astro-ph.EP; astro-ph.IM
Abstract :
[en] Context. HD 98800 is a young (∼10 Myr old) and nearby (∼45 pc) quadruple system, composed of two spectroscopic binaries orbiting around each other (AaAb and BaBb), with a gas-rich disk in polar configuration around BaBb. While the orbital parameters of BaBb and AB are relatively well constrained, this is not the case for AaAb. A full characterisation of this quadruple system can provide insights on the formation of such a complex system. Aims. The goal of this work is to determine the orbit of the AaAb subsystem and refine the orbital solution of BaBb using multi-epoch interferometric observations with the Very Large Telescope Interferometer PIONIER and radial velocities. Methods. The PIONIER observations provide relative astrometric positions and flux ratios for both AaAa and BaBb subsystems. Combining the astrometric points with radial velocity measurements, we determine the orbital parameters of both subsystems. Results. We refined the orbital solution of BaBb and derived, for the first time, the full orbital solution of AaAb. We confirmed the polar configuration of the circumbinary disk around BaBb. From our solutions, we also inferred the dynamical masses of AaAb (MAa=0.93±0.09 and MAb=0.29±0.02M). We also revisited the parameters of the AB outer orbit. Conclusions. The orbital parameters are relevant to test the long-term stability of the system and to evaluate possible formation scenarios of HD 98800. Using the N-body simulation, we show that the system should be dynamically stable over thousands of orbital periods and that it made preliminary predictions for the transit of the disk in front of AaAb which is estimated to start around 2026. We discuss the lack of a disk around AaAb, which can be explained by the larger X-ray luminosity of AaAb, promoting faster photo-evaporation of the disk. High-resolution infrared spectroscopic observations would provide radial velocities of Aa and Ab (blended lines in contemporary observations), which would allow us to calculate the dynamical masses of Aa and Ab independently of the parallax of BaBb. Further monitoring of other hierarchical systems will improve our understanding of the formation and dynamical evolution of these kinds of systems.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Zúñiga Fernández, Sebastián Gaspar ; Université de Liège - ULiège > Astrobiology ; Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile ; European Southern Observatory, Santiago de Chile, Chile ; Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile
Olofsson, J.; Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile ; Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile
Bayo, A.; Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile ; Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile
Haubois, X.; European Southern Observatory, Santiago de Chile, Chile
Corral-Santana, J.M.; European Southern Observatory, Santiago de Chile, Chile
Lopera-Mejía, A.; Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Valparaíso, Chile
Ronco, M.P.; Núcleo Milenio de Formación Planetaria (NPF), Valparaíso, Chile ; Instituto de Astrofísica - Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile
Gallenne, A.; Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences, Warszawa, Poland ; Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile ; Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS Umi 3386), Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Kennedy, G.M.; Department of Physics, University of Warwick, Coventry, United Kingdom
Berger, J.-P.; Université Grenoble Alpes, Cnrs, Ipag, Grenoble, France
Language :
English
Title :
The HD 98800 quadruple pre-main sequence system: Towards full orbital characterisation using long-baseline infrared interferometry
ESO - European Southern Observatory ANID - Agencia Nacional de Investigación y Desarrollo FONDECYT - National Fund for Scientific and Technological Development
Funding text :
Acknowledgements. The authors would like to thank the anonymous referee for constructive comments that helped to improve the content and clarity of this paper. S.Z.-F. acknowledges financial support from the European Southern Observatory via its studentship program and ANID via PFCHA/Doctorado Nacional/2018-21181044. J.O. acknowledges support from the Universidad de Valparaíso and from Fondecyt (grant 1180395). S.Z.-F., A.B., J.O. and M.P.R. acknowledge support by ANID, – Millennium Science Initiative Program – NCN19_171. A.B. acknowledges support from Fondecyt (grant 1190748). M.P.R. acknowledges support from Fondecyt (grant 3190336). G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow. This research made use of exoplanet (Foreman-Mackey et al. 2020) and its dependencies (Astropy Collaboration 2013, 2018; Salvatier et al. 2016; Theano Development Team 2016). This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/ web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of VOSA (Bayo et al. 2008), developed under the Spanish Virtual Observatory project supported by the Spanish MINECO through grant AyA2017-84089. This research has made use of NASA’s Astrophysics Data System.
Commentary :
Accepted for publication in Astronomy \& Astrophysiscs journal
(01/09/2021)
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