The magnetosphere of the close accreting PMS binary V4046 Sgr
1 School of Physics & Astronomy, University of St Andrews, St Andrews, KY16 9SS U.K.
2 Freytagstr. 7, D-79114 Freiburg i.Br., Germany
3 UPS-Toulouse/CNRS-INSU, Inst. de Recherche en Astro. et Planétologie, F-31400 Toulouse, France
4 ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany
5 Institut d’Astrophysique de Paris, 98bis bd Arago, FR-75014 Paris, France
6 Obs. de Paris, LESIA, 5, place Jules Janssen, F-92195 Meudon Principal Cedex, France
7 Dept. de Fìsica - UFMG, Av. Antônio Carlos, 6627 30270-901 Belo Horizonte MG, Brazil
8 INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, I-90134 Palermo Italy
9 ISDC Data Center for Astrophysics Univ. of Geneva, CH-1290 Versoix Switzerland
10 UJF-Grenoble 1/CNRS-INSU, IPAG, UMR 5274, F-38041, Grenoble, France
11 Dept. of Astrophysics, University of Vienna, Türkenschanzstrasse 17, A-1180, Vienna, Austria
12 MIT, Kavli Inst. for Astrophysics & Space Research, Cambridge, MA 02139, U.S.A.
13 CIS, Rochester Inst. of Technology, 54 Lomb Memorial Drive, Rochester, MA 02139, U.S.A.
14 INAF-Arcetri Astrophysical Observatory, Largo Enrico Fermi 5, I - 50125, Florence, Italy
15 Dept. of Physics, Royal Military College of Canada, Kingston, K7K 7B4, Canada
a e-mail: firstname.lastname@example.org
Published online: 8 January 2014
V4046 Sagittarii AB is a close short-period classical T Tauri binary. It is a circularised and synchronised system accreting from a circumbinary disk. In 2009 it was observed as part of a coordinated program involving near-simultaneous spectropolarimetric observations with ESPaDOnS at the Canada-France-Hawai’i Telescope and high-resolution X-ray observations with XMM-Newton. Magnetic maps of each star were derived from Zeeman-Doppler imaging. After briefly highlighting the most significant observational findings, we present a preliminary 3D model of the binary magnetosphere constructed from the magnetic maps using a newly developed binary magnetic field extrapolation code. The large-scale fields (the dipole components) of both stars are highly tilted with respect to their rotation axes, and their magnetic fields are linked.
© Owned by the authors, published by EDP Sciences, 2014
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