Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha
Article
Article Title | Surface magnetic fields on two accreting T Tauri stars: CV Cha and CR Cha |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Hussain, G. A. J. (Author), Collier Cameron, A. (Author), Jardine, M. M. (Author), Dunstone, N. (Author), Ramirez Velez, J. (Author), Stempels, H. C. (Author), Donati, J.-F. (Author), Semel, M. (Author), Aulanier, G. (Author), Harries, T. (Author), Bouvier, J. (Author), Dougados, C. (Author), Ferreira, J. (Author), Carter, B. D. (Author) and Lawson, W. A. (Author) |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 398 (1), pp. 189-200 |
Number of Pages | 12 |
Year | 2009 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1111/j.1365-2966.2009.14881.x |
Web Address (URL) | https://academic.oup.com/mnras/article/398/1/189/1094128 |
Abstract | 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. |
Keywords | stars; formation; imaging; individual; CR Cha; CV Cha; magnetic fields; open clusters and associations; Chamaeleon I |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
370109. Tropospheric and stratospheric physics | |
510402. Condensed matter imaging | |
401304. Photogrammetry and remote sensing | |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2009 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | European Southern Observatory (ESO), Germany |
University of St Andrews, United Kingdom | |
Paris Sciences and Letters University, France | |
Institute for Research in Astrophysics and Planetology, France | |
Laboratory of Space Science and Astrophysical Instrumentation, France | |
University of Exeter, United Kingdom | |
Institute of Planetology and Astrophysics of Grenoble, France | |
Department of Biological and Physical Sciences | |
University of New South Wales |
https://research.usq.edu.au/item/9z333/surface-magnetic-fields-on-two-accreting-t-tauri-stars-cv-cha-and-cr-cha
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