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Abstract
Understanding how cool stars produce magnetic fields within their interiors is crucial for predicting the impact of such fields, such as the activity cycle of the Sun. In this respect, studying fully convective stars enables us to investigate the role of convective zones in magnetic field generation. We produced a magnetic map of a rapidly rotating, very-low-mass, fully convective dwarf through tomographic imaging from time series of spectropolarimetric data. Our results, which demonstrate that fully convective stars are able to trigger axisymmetric large-scale poloidal fields without differential rotation, challenge existing theoretical models of field generation in cool stars.
Original language | English |
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Pages (from-to) | 633-635 |
Number of pages | 3 |
Journal | Science |
Volume | 311 |
Issue number | 5761 |
DOIs | |
Publication status | Published - 3 Feb 2006 |
Keywords
- T-TAURI STARS
- ACTIVE STARS
- M-DWARFS
- SOLAR DYNAMO
- ROTATION
- FIELD
- RECONSTRUCTION
- GENERATION
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Dive into the research topics of 'The Large-Scale Axisymmetric Magnetic Topology of a Very-Low-Mass Fully Convective Star'. Together they form a unique fingerprint.Projects
- 1 Finished
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Astrophysics at St Andrews: Astrophysics at St.Andrews
Cameron, A. C. (PI) & Horne, K. D. (CoI)
1/04/06 → 31/03/11
Project: Standard