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The evolution of surface magnetic fields in young solar-type stars

Published online by Cambridge University Press:  07 August 2014

C. P. Folsom ,
P. Petit ,
J. Bouvier ,
J.-F. Donati  and
J. Morin
C. P. Folsom
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Toulouse, France email: colin.folsom@irap.omp.eu
P. Petit
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Toulouse, France email: colin.folsom@irap.omp.eu
J. Bouvier
Affiliation:
Institut de Planétologie et d'Astrophysique de Grenoble, France
J.-F. Donati
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Toulouse, France email: colin.folsom@irap.omp.eu
J. Morin
Affiliation:
Institute of Astrophysics, Georg-August-University, Göttingen, Germany
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Abstract

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The surface rotation rates of young solar-type stars decrease rapidly with age from the end of the pre-main sequence though the early main sequence. This suggests that there is also an important change in the dynamos operating in these stars, which should be observable in their surface magnetic fields. Here we present early results in a study aimed at observing the evolution of these magnetic fields through this critical time period. We are observing stars in open clusters and stellar associations to provide precise ages, and using Zeeman Doppler Imaging to characterize the complex magnetic fields. Presented here are results for six stars, three in the in the β Pic association (~10 Myr old) and three in the AB Dor association (~100 Myr old).

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 110 - 111
Copyright
Copyright © International Astronomical Union 2014 

References

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