The magnetic fields of accreting T Tauri stars

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

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

1 Citation (Scopus)

Abstract

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 BP 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 publicationProceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
EditorsH. C. Stemples
PublisherAmerican Institute of Physics
Pages71-76
Number of pages6
Volume1094
ISBN (Print)9780735406278
DOIs
Publication statusPublished - 25 Feb 2009

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