Issue |
A&A
Volume 688, August 2024
|
|
---|---|---|
Article Number | A102 | |
Number of page(s) | 16 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/202348470 | |
Published online | 07 August 2024 |
Orbital dynamics in the GG Tau A system: Investigating its enigmatic disc
1
European Southern Observatory (ESO),
Karl-Schwarzschild-Strasse 2,
85748
Garching bei Munchen,
Germany
2
INAF, Osservatorio Astrofísico di Arcetri,
50125
Firenze,
Italy
e-mail: claudia.toci@eso.org
3
Dipartimento di Fisica, Università degli Studi di Milano,
Via Celoria 16,
20133
Milano,
Italy
4
Univ. Grenoble Alpes, CNRS, IPAG,
38000
Grenoble,
France
5
Department of Astronomy, University of California,
Berkeley,
CA
94720,
USA
6
Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS,
Centre de Recherche Astrophysique de Lyon UMR5574,
69230
Saint-Genis-Laval,
France
7
Dipartimento di Matematica, Università degli Studi di Milano,
Via Saldini 50,
20133
Milano,
Italy
8
Faculty of Aerospace Engineering, Delft University of Technology,
Kluyverweg 1,
2629 HS
Delft,
The Netherlands
Received:
2
November
2023
Accepted:
8
April
2024
Context. GG Tau is one of the most studied young multiple stellar systems: GG Tau A is a hierarchical triple surrounded by a massive disc and its companion, GG Tau B, is also a binary. Despite numerous observational attempts, a comprehensive understanding of the geometry of the GG Tau A system is still elusive. Given the significant role of dynamical interactions in shaping the evolution of these systems, it is relevant to characterise the stellar orbits and the discs’ properties.
Aims. To determine the best orbital configuration of the GG Tau A system and its circumtriple disc, we provide new astrometric measures of the system and we run a set of hydrodynamical simulations with two representative orbits to test how they impact a disc composed of dust and gas.
Methods. We tested the dynamical evolution of the two scenarios on short and long timescales. We obtained synthetic flux emission from our simulations at different timescales and we compared them with multi-wavelength observations of 1300 µm ALMA dust continuum emission and 1.67 µm SPHERE dust scattering to infer the most likely orbital arrangement.
Results. We extend the analysis of the binary orbital parameters using six new epochs from archival data, showing that the current measurements alone (and future observations coming in the next 5–10 yr) are not capable of fully breaking the degeneracy between families of coplanar and misaligned orbits, but finding that a modest misalignment is probable. We find that the timescale for the onset of the disc eccentricity growth, τecc, is a fundamental timescale for the morphology of the system. Results from the numerical simulations obtained using the representative coplanar and misaligned (∆θ = 30°) orbits show that the best match between the position of the stars, the cavity size, and the dust ring size of GG Tau A is obtained with the misaligned configuration on timescales shorter than τecc. The results exhibit an almost circular cavity and dust ring, favouring slightly misaligned (∆θ ~ 10–30°) low-eccentricity (e ~ 0.2–0.4) orbits. However, for both scenarios, the cavity size and its eccentricity quickly grow for timescales longer than τecc and the models do not reproduce the observed morphology anymore. This implies that either the age of the system is shorter than τecc or that the disc eccentricity growth is not triggered or dissipated in the system. This finding raises questions about the future evolution of the GG Tau A system and, more generally, the time evolution of eccentric binaries and their circumbinary discs.
Key words: hydrodynamics / astrometry / protoplanetary disks / binaries close / stars: individual: GG Tau A
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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