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Time variable funnel flows

Published online by Cambridge University Press:  01 May 2007

Silvia H. P. Alencar
Silvia H. P. Alencar*
Affiliation:
Departamento de Física – ICEx – UFMG, CP 702, 31270-901, Belo Horizonte, MG, Brazil email: silvia@fisica.ufmg.br
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Abstract

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Magnetospheric accretion models are the current consensus to explain the main observed characteristics of classical T Tauri stars. In recent years the concept of a static magnetosphere has been challenged by synoptic studies of classical T Tauri stars that show strong evidence for the accretion process to be dynamic on several timescales and governed by changes in the magnetic field configuration. At the same time numerical simulation results predict evolving funnel flows due to the interaction between the stellar magnetosphere and the inner disk region. In this contribution we will focus on the main recent observational evidences for time variable funnel flows and compare them with model predictions.

Keywords

Stars: pre–main-sequencestars: magnetic fieldscircumstellar matteraccretion
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 71 - 82
Copyright
Copyright © International Astronomical Union 2007

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