Abstract
Current magnetic-accretion models for classical T Tauri stars rely on a strong, dipolar magnetic field of stellar origin to funnel the disk material onto the star and assume a steady-state. In this paper, I critically examine the physical basis of these models in light of the observational evidence and our knowledge of magnetic fields in low-mass stars and find it lacking. I also argue that magnetic accretion onto these stars is inherently a time-dependent problem and that a steady state is not warranted.
Finally, directions for future work toward fully consistent models are pointed out.
Export citation and abstract BibTeX RIS