The magnetic field geometry of cool stars
Creators
- See, Victor1
- Jardine, Moira1
- Vidotto, Aline2
- Donati, Jean-Francois3
- Folsom, Colin4
- Boro Saikia, Sudeshna5
- Bouvier, Jerome4
- Fares, Rim6
- Gregory, Scott1
- Hussain, Gaitee7
- Jeffers, Sandra5
- Marsden, Stephen8
- Morin, Julien9
- Moutou, Claire10
- do Nascimento Jr, Jose-Dias11
- Petit, Pascal3
- Rosen, Lisa12
- Waite, Ian8
- 1. University of St Andrews
- 2. Trinity College Dublin
- 3. University of Toulouse
- 4. University of Grenoble
- 5. University of Goettingen
- 6. University of Catania
- 7. European Southern Observatory
- 8. University of Southern Queensland
- 9. University of Montpellier
- 10. Canada-France-Hawaii Telescope Corporation
- 11. Center for Astrophysics
- 12. Uppsala University
Description
Zeeman-Doppler imaging has been used to map the large-scale surface magnetic fields of cool stars across a wide range of stellar masses and rotation periods. The derived field geometries are surprising, with many stars showing strong azimuthal fields that are not observed on the Sun. In this poster, using ~100 magnetic maps of over 50 stars, we present results showing how the magnetic field geometry of cool stars varies as a function of fundamental parameters. The stellar mass, and hence internal structure, critically influences the field geometry, although this is modified by the stellar rotation rate. We discuss the implications of these results for dynamo theory and the nature of stellar magnetic activity.
Notes
Files
CS19Poster.pdf
Files
(8.3 MB)
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