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The wind and the magnetospheric accretion onto the T Tauri star S Coronae Australis at sub-au resolution

R. Garcia Lopez K. Perraut 1 A. Caratti O Garatti B. Lazareff 1 J. Sanchez-Bermudez 2 M. Benisty 1 C. Dougados 1 L. Labadie 1 W. Brandner 3 J. Garcia 4 Th. Henning 3 P. Ray 5 R. Abuter 2 A. Amorim 6 N. Anugu J. Berger H. Bonnet A. Buron P. Caselli 7 Y. Clenet 8 Vincent Coudé Du Forestol 8 W. de Wit C. Deen F. Delplancke-Ströbele J. Dexter A. Eckart 9 F. Eisenhauer 10 C. Garcia E. Gendron 8 R. Genzel 10 S. Gillessen 10 X. Haubois M. Haug F. Haussmann S. Hippler Z. Hubert 8 A. Hummel 11 M. Horrobin 12 L. Jocou 1 S. Kellner P. Kervella 8 M. Kulas J. Kolb S. Lacour 13 B. Le Bouquin P. Lena 8 M. Lippa A. Merand 14 E. Müller T. Ott 15 J. Panduro T. Paumard 8 G. Perrin 8 O. Pfuhl 10 A. Ramírez 16 C. Rau 17 R. Rohloff G. Rousset 8 S. Scheithauer M. Scholler 18 C. Straubmeier 19 E. Sturm 10 W. Thi E. van Dishoeck 20 F. Vincent 8 I. Waisberg I. Wank E. Wieprecht 21 M. Wiest E. Wiezorrek 10 J. Woillez 2 S. Yazici G. Zins 1 
Abstract : Aims. To investigate the inner regions of protoplanetary discs, we performed near-infrared interferometric observations of the classical T Tauri binary system S CrA.Methods. We present the first VLTI-GRAVITY high spectral resolution (R ~ 4000) observations of a classical T Tauri binary, S CrA (composed of S CrA N and S CrA S and separated by ~1.̋4), combining the four 8m telescopes in dual-field mode. Results. Our observations in the near-infrared K-band continuum reveal a disc around each binary component, with similar half-flux radii of about 0.1 au at d ~ 130 pc, inclinations (i = 28 ± 3° and i = 22 ± 6°), and position angles (PA = 0°± 6° and PA = –2°± 12°), suggesting that they formed from the fragmentation of a common disc. The S CrA N spectrum shows bright He i and Brγ line emission exhibiting inverse P Cygni profiles, typically associated with infalling gas. The continuum-compensated Brγ line visibilities of S CrA N show the presence of a compact Brγ emitting region whose radius is about ~0.06 au, which is twice as big as the truncation radius. This component is mostly tracing a wind. Moreover, a slight radius change between the blue- and red-shifted Brγ line components is marginally detected.Conclusions. The presence of an inverse P Cygni profile in the He i and Brγ lines, along with the tentative detection of a slightly larger size of the blue-shifted Brγ line component, hint at the simultaneous presence of a wind and magnetospheric accretion in S CrA N.
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R. Garcia Lopez, K. Perraut, A. Caratti O Garatti, B. Lazareff, J. Sanchez-Bermudez, et al.. The wind and the magnetospheric accretion onto the T Tauri star S Coronae Australis at sub-au resolution. Astronomy and Astrophysics - A&A, EDP Sciences, 2017, 608, pp.A78. ⟨10.1051/0004-6361/201731058⟩. ⟨obspm-02190736⟩



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