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The ejection-accretion connection in young stars: Testing MHD disk winds

Published online by Cambridge University Press:  21 October 2010

S. Cabrit ,
J. Ferreira ,
C. Dougados  and
P. Garcia
S. Cabrit
Affiliation:
LERMA, Observatoire de Paris, UMR 8112 du CNRS, 61 Av. de l'Observatoire, F-75014 Paris. email: [email protected]
J. Ferreira
Affiliation:
Laboratoire d'Astrophysique de l'Observatoire de Grenoble, UMR 5521 du CNRS, F-38041 Grenoble Cedex. email: [email protected], [email protected]
C. Dougados
Affiliation:
Laboratoire d'Astrophysique de l'Observatoire de Grenoble, UMR 5521 du CNRS, F-38041 Grenoble Cedex. email: [email protected], [email protected]
P. Garcia
Affiliation:
Laboratoire d'Astrophysique de l'Observatoire de Grenoble, UMR 5521 du CNRS, F-38041 Grenoble Cedex. email: [email protected], [email protected] Universidade do Porto, Faculdade de Engenharia, Laboratório de Sistemas, Instrumentação e Modelação em Ciências e Tecnologias do Ambiente e do Espaço, P-4200-465 Porto, Portugal email: [email protected]
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Abstract

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Jets are ubiquitous in young accreting stars at all evolutionary stages, from deeply embedded protostars aged less than 0.1Myr to optically revealed 10Myr old T Tauri stars. The similar jet collimation at all ages is shown to require an effective magnetic collimation within the inner disk regions (inside 20 AU). This fact, and the high ejection to accretion ratio ≃10%, appear to favor the presence of MHD disk winds. Ejection out to > 0.1 AU could explain the velocity drop and rotation signatures across the jets, and their dust and molecular content.

Keywords

accretion disksMHDstars: pre–main-sequenceISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 261 - 262
Copyright
Copyright © International Astronomical Union 2010

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