The magnetic fields of accreting T Tauri stars

S. G. Gregory, S. P. Matt, J. -F. Donati, M. Jardine

Research output: Chapter in Book/Report/Conference proceedingConference contribution

1 Citation (Scopus)


Models of magnetospheric accretion on to classical T Tauri stars often assume that the stellar magnetic field is a simple dipole. Recent Zeeman-Doppler imaging studies of V2129 Oph and RP Tau have shown however that their magnetic fields are more complex. V2129 Oph is a high mass T Tauri star and despite its young age is believed to have already developed a radiative core. In contrast to this, the lower mass BP Tau is likely to be completely convective. As the internal structure and therefore the magnetic field generation process is different in both stars, it is of particular interest to compare the structure of their magnetic fields obtained by field extrapolation from magnetic surface maps. We compare both field structures to mulitpole magnetic fields, and calculate the disk truncation radius for both systems. We find that by considering magnetic fields with a realistic degree of complexity, the disk is truncated at, or within, the radius obtained for dipole fields.

Original languageEnglish
Title of host publicationCool stars, stellar systems and the sun
Subtitle of host publication15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, St. Andrews, Scotland, 21-25 July 2008
EditorsE Stempels
Place of PublicationMelville, New York
PublisherAmerican Institute of Physics
Number of pages6
ISBN (Print)978-0-7354-0627-8
Publication statusPublished - Feb 2009

Publication series

NameAIP Conference Proceedings
ISSN (Print)0094-243X


  • Stellar magnetospheres
  • Stellar magnetic fields
  • T Tauri stars
  • Magnetospheric accretion
  • V2129-Oph
  • BP Tau


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