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The X-wind Model

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Protostellar Jets in Context

Part of the book series: Astrophysics and Space Science Proceedings ((ASSSP))

Abstract

Based on the principle of magneto-centrifugal acceleration, the interaction of an electrically conducting accretion disk with the magnetosphere of a young star will naturally give rise to X-winds and funnel flows. A distinguishing feature of the X-wind model is the trapped flux in a small region at the inner edge of the disk, where both the X-wind and the funnel flow originate. We will review some of the theoretical developments of the X-wind model and how some of its predictions can be tested by observation.

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Author information

Authors and Affiliations

  1. Academia Sinica, Institute of Astronomy and Astrophysics, Taipei, Taiwan

    Mike J. Cai

Authors
  1. Mike J. Cai
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Corresponding author

Correspondence to Mike J. Cai .

Editor information

Editors and Affiliations

  1. Dept. Physics, University of Athens, Panepistimiopolis, Athens, 157 84, Greece

    Kanaris Tsinganos

  2. Astronomy & Astrophysics Section, Dublin Institute for Advanced Studies, Fitzwilliam Place 31, Dublin, Ireland

    Tom Ray

  3. Dept. Physics, University of Athens, Panepistimiopolis, Athens, 157 84, Greece

    Matthias Stute

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© 2009 Springer-Verlag Berlin Heidelberg

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Cai, M.J. (2009). The X-wind Model. In: Tsinganos, K., Ray, T., Stute, M. (eds) Protostellar Jets in Context. Astrophysics and Space Science Proceedings. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-00576-3_18

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  • DOI: https://doi.org/10.1007/978-3-642-00576-3_18

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  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-642-00575-6

  • Online ISBN: 978-3-642-00576-3

  • eBook Packages: Physics and AstronomyPhysics and Astronomy (R0)

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