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The role of magnetic fields in pre-main sequence stars

Published online by Cambridge University Press:  07 August 2014

Gaitee A. J. Hussain  and
Evelyne Alecian
Gaitee A. J. Hussain
Affiliation:
ESO, Karl-Schwarzschild-Strasse 2, D-85748, Garching bei MünchenGermany email: [email protected]
Evelyne Alecian
Affiliation:
UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG)UMR 5274, Grenoble, F-38041, France email: [email protected] LESIA, UMR 8109 du CNRS, Observatoire de Paris, UPMC, Université Paris Diderot, 5 place Jules Janssen, F-92195 Meudon Cedex, France
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Abstract

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Strong, kilo-Gauss, magnetic fields are required to explain a range of observational properties in young, accreting pre-main sequence (PMS) systems. We review the techniques used to detect magnetic fields in PMS stars. Key results from a long running campaign aimed at characterising the large scale magnetic fields in accreting T Tauri stars are presented. Maps of surface magnetic flux in these systems can be used to build 3-D models exploring the role of magnetic fields and the efficiency with which magnetic fields can channel accretion from circumstellar disks on to young stars. Long-term variability in T Tauri star magnetic fields strongly point to a dynamo origin of the magnetic fields. Studies are underway to quantify how changes in magnetic fields affect their accretion properties. We also present the first results from a new programme that investigates the evolution of magnetic fields in intermediate mass (1.5–3M⊙) pre-main sequence stars as they evolve from being convective T Tauri stars to fully radiative Herbig AeBe stars.

Keywords

stars: activitystars: accretingstars: circumstellar matterstars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 25 - 37
Copyright
Copyright © International Astronomical Union 2014 

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