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2007MNRAS.380.1297D - Mon. Not. R. Astron. Soc., 380, 1297-1312 (2007/October-1)
Magnetic fields and accretion flows on the classical T Tauri star V2129 Oph.
DONATI J.-F., JARDINE M.M., GREGORY S.G., PETIT P., BOUVIER J., DOUGADOS C., MENARD F., CAMERON A.C., HARRIES T.J., JEFFERS S.V. and PALETOU F.
Abstract (from CDS):
We reconstruct the large-scale magnetic topology at the surface of V2129 Oph from both sets of Zeeman signatures simultaneously. We find it to be rather complex, with a dominant octupolar component and a weak dipole of strengths 1.2 and 0.35 kG, respectively, both slightly tilted with respect to the rotation axis. The large-scale field is anchored in a pair of 2-kG unipolar radial field spots located at high latitudes and coinciding with cool dark polar spots at photospheric level. This large-scale field geometry is unusually complex compared to those of non-accreting cool active subgiants with moderate rotation rates.
As an illustration, we provide a first attempt at modelling the magnetospheric topology and accretion funnels of V2129 Oph using field extrapolation. We find that the magnetosphere of V2129 Oph must extend to about 7R* to ensure that the footpoints of accretion funnels coincide with the high-latitude accretion spots on the stellar surface. It suggests that the stellar magnetic field succeeds in coupling to the accretion disc as far out as the corotation radius, and could possibly explain the slow rotation of V2129 Oph. The magnetospheric geometry we derive qualitatively reproduces the modulation of Balmer lines and produces X-ray coronal fluxes typical of those observed in cTTSs.
Abstract Copyright: 2007 The Authors. Journal compilation © 2007 RAS
Journal keyword(s): accretion, accretion discs - techniques: spectroscopic - stars: formation - stars: individual: V2129 Oph - stars: magnetic fields - stars: rotation
Simbad objects: 4
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