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Séminaire MHD (SEMHD)

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The magneto-spheric accretion onto young objects: An observational review
Jérôme Bouvier (LAOG, Grenoble)

2 février 2009

Young solar-type stars, the so-called T Tauri stars, possess strong and complex magnetic fields, whose strength and topology are now directly measured through spectropolarimetric techniques. These strong fields disrupt the inner accretion disk over a distance of a few stellar radii, thus leading to magnetic funnel flows connecting the inner edge of the disk to the stellar surface, to hot spots which are the signature of accretion shocks as the free-falling gas hits the stellar surface near the magnetic poles, and to an inner disk warp as the gas and dust in the inner disk are lifted up away from the central plane by the large-scale stellar magnetic field. I will provide a summary of the observational evidence available so far for strong magnetic fields in young stars, inner disk truncation, accretion funnel flows, accretion shocks, and associated outflows. I will also discuss the evidence for instabilities in these MHD process which are observed to be strongly variable on timescales ranging from a few hours to several years. Eventually, I will discuss the implications of magnetospheric accretion-ejection processes for the angular momentum evolution of young stars.
Bibliographie :
– Bouvier J., Alencar S., Harries T., Johans-Krull C.M., Romanova M.M., 2007, "Magnetospheric accretion in classical T Tauri stars", in Protostars & Planets V, eds B. Reipurth, D. Jewitt, and K. Keil, p. 479.
– Bouvier J., Appenzeller I., eds, 2007, Star-disk interaction in young stars, IAU Symposium 243, Cambridge University Press.

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Non disponible Jérôme Bouvier (LAOG, Grenoble)
Jérome Bouvier est directeur de recherche CNRS au Laboratoire d’astrophysique de l’observatoire de Grenoble.

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