Journal Article

A radiation-driven disc wind model for massive young stellar objects

Janet E. Drew, Daniel Proga and James M. Stone

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 296, issue 1, pages L6-L10
Published in print May 1998 | ISSN: 0035-8711
Published online May 1998 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1046/j.1365-8711.1998.01438.x
A radiation-driven disc wind model for massive young stellar objects

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A radiation-driven disc wind model is proposed that offers great promise of explaining the extreme mass-loss signatures of massive young stellar objects (the BN-type objects and more luminous Herbig Be stars). It is argued that the dense low-velocity winds associated with young late O/early B stars would be the consequence of continuing optically thick accretion on to them. The launch of outflow from a Keplerian disc allows wind speeds of ∼200 km s−1 that are substantially less than the escape speed from the stellar surface. The star itself is not required to be a rapid rotator. Disc irradiation is taken into account in the hydrodynamical calculation presented, and identified as an important issue both observationally and from the dynamical point of view.

Keywords: accretion; accretion discs; hydrodynamics; methods: numerical; circumstellar matter; stars: mass-loss; stars: pre-main-sequence

Journal Article.  0 words. 

Subjects: Astronomy and Astrophysics

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