The role of magnetic fields in pre-main sequence stars
arXiv:1402.7130 · doi:10.1017/S1743921314001653
Abstract
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 (1.5-3 Msun) pre-main sequence stars as they evolve from being convective T Tauri stars to fully radiative Herbig AeBe stars.
13 pages, 6 figures, conference proceedings
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- The Role of Magnetic Fields in Protostellar Outflows and Star Formation
- Jets from Young Stars
- The influence of radiative core growth on coronal X-ray emission from pre-main sequence stars
- The Effect of a Magnetic Field on the Dynamics of Debris Discs Around White Dwarfs
- Inactive longitude and superflare in the active single-lined pre-main sequence binary V2279 Cyg