Ongoing flyby in the young multiple system UX Tauri

F. Ménard; N. Cuello; C. Ginski; G. van der Plas; M. Villenave; J.-F. Gonzalez; C. Pinte; M. Benisty; A. Boccaletti; D. J. Price; Y. Boehler; S. Chripko; J. de Boer; C. Dominik; A. Garufi; R. Gratton; J. Hagelberg; Th. Henning; M. Langlois; A. L. Maire; P. Pinilla; G. J. Ruane; H. M. Schmid; R. G. van Holstein; A. Vigan; A. Zurlo; N. Hubin; A. Pavlov; S. Rochat; J.-F. Sauvage; E. Stadler

doi:10.1051/0004-6361/202038356

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Volume 639 (July 2020)

A&A, 639 (2020) L1

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Issue		A&A Volume 639, July 2020


Article Number		L1
Number of page(s)		7
Section		Letters to the Editor
DOI		https://doi.org/10.1051/0004-6361/202038356
Published online		02 July 2020

A&A 639, L1 (2020)

Letter to the Editor

Ongoing flyby in the young multiple system UX Tauri^⋆

F. Ménard¹, N. Cuello¹^,2^,3, C. Ginski⁴^,5, G. van der Plas¹, M. Villenave¹^,6, J.-F. Gonzalez³, C. Pinte⁷^,1, M. Benisty¹, A. Boccaletti⁸, D. J. Price⁷, Y. Boehler¹, S. Chripko⁹, J. de Boer⁵, C. Dominik⁴, A. Garufi¹⁰, R. Gratton¹¹, J. Hagelberg¹², Th. Henning¹³, M. Langlois³, A. L. Maire¹⁴^,13, P. Pinilla¹³, G. J. Ruane¹⁵, H. M. Schmid¹⁶, R. G. van Holstein⁵^,6, A. Vigan¹⁷, A. Zurlo¹⁷^,18^,19, N. Hubin²⁰, A. Pavlov¹³, S. Rochat¹, J.-F. Sauvage²¹^,17 and E. Stadler¹

¹ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
e-mail: francois.menard@univ-grenoble-alpes.fr
² Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile
³ Univ Lyon, Univ Claude Bernard Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69230 Saint-Genis-Laval, France
⁴ Sterrenkundig Instituut Anton Pannekoek, Science Park 904, 1098 XH Amsterdam, The Netherlands
⁵ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
⁶ European Southern Observatory, Alonso de Córdova 3107, Casilla 19001 Vitacura, Santiago, Chile
⁷ School of Physics and Astronomy, Monash University, Clayton, Vic 3800, Australia
⁸ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Univ. Paris Diderot, Sorbonne Paris Cité, 5 place Jules Janssen, 92195 Meudon, France
⁹ CECI, Université de Toulouse, CNRS, CERFACS, Toulouse, France
¹⁰ INAF, Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy
¹¹ INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
¹² Geneva Observatory, University of Geneva, Chemin des Mailettes 51, 1290 Versoix, Switzerland
¹³ Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
¹⁴ STAR Institute, Université de Liège, Allée du Six Août 19c, 4000 Liège, Belgium
¹⁵ Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109, USA
¹⁶ Institute for Particle Physics and Astrophysics, ETH Zurich, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland
¹⁷ Aix Marseille Université, CNRS, CNES, LAM, Marseille, France
¹⁸ Núcleo de Astronomía, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile
¹⁹ Escuela de Ingeniería Industrial, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejercito 441, Santiago, Chile
²⁰ European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
²¹ DOTA, ONERA, Université Paris Saclay, 91123 Palaiseau, France

Received: 5 May 2020
Accepted: 1 June 2020

Abstract

We present observations of the young multiple system UX Tauri to look for circumstellar disks and for signs of dynamical interactions. We obtained SPHERE/IRDIS deep differential polarization images in the J and H bands. We also used ALMA archival CO data. Large extended spirals are well detected in scattered light coming out of the disk of UX Tau A. The southern spiral forms a bridge between UX Tau A and C. These spirals, including the bridge connecting the two stars, all have a CO (3–2) counterpart seen by ALMA. The disk of UX Tau C is detected in scattered light. It is much smaller than the disk of UX Tau A and has a major axis along a different position angle, suggesting a misalignment. We performed PHANTOM SPH hydrodynamical models to interpret the data. The scattered light spirals, CO emission spirals and velocity patterns of the rotating disks, and the compactness of the disk of UX Tau C all point to a scenario in which UX Tau A has been perturbed very recently (∼1000 years) by the close passage of UX Tau C.

Key words: protoplanetary disks / circumstellar matter / stars: pre-main sequence / binaries: general

^⋆

Movies associated to Fig. 3 are available at https://www.aanda.org

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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Ongoing flyby in the young multiple system UX Tauri⋆

Ongoing flyby in the young multiple system UX Tauri^⋆