Hussain, G. A. J. and Collier Cameron, A. and Jardine, M. M. and Dunstone, N. and Ramirez Velez, J. and Stempels, H. C. and Donati, J.-F. and Semel, M. and Aulanier, G. and Harries, T. and Bouvier, J. and Dougados, C. and Ferreira, J. and Carter, B. D. and Lawson, W. A. (2009) Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha. Monthly Notices of the Royal Astronomical Society, 398 (1). pp. 189-200. ISSN 0035-8711
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Identification Number or DOI: doi: 10.1111/j.1365-2966.2009.14881.x
We have produced brightness and magnetic field maps of the surfaces of CV Cha and CR Cha: two actively accreting G- and K-type T Tauri stars in the Chamaeleon I star-forming cloud with ages of 3–5 Myr. Our magnetic field maps show evidence for strong, complex multipolar fields similar to those obtained for young rapidly rotating main-sequence stars. Brightness maps indicate the presence of dark polar caps and low-latitude spots – these brightness maps are very similar to those obtained for other pre-main-sequence and rapidly rotating main-sequence stars. Only two other classical T Tauri stars have been studied using similar techniques so far: V2129 Oph and BP Tau. CV Cha and CR Cha show magnetic field patterns that are significantly more complex than those recovered for BP Tau, a fully convective T Tauri star. We discuss possible reasons for this difference and suggest that the complexity of the stellar magnetic field is related to the convection zone; with more complex fields being found in T Tauri stars with radiative cores (V2129 Oph, CV Cha and CR Cha). However, it is clearly necessary to conduct magnetic field studies of T Tauri star systems, exploring a wide range of stellar parameters in order to establish how they affect magnetic field generation, and thus how these magnetic fields are likely to affect the evolution of T Tauri star systems as they approach the main sequence.
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