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

J.E. Drew, D. Proga, J.M. Stone

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    A radiation-driven disk 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 onto them. The launch of outflow from a Keplerian disk 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. Disk 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.
    Original languageEnglish
    Pages (from-to)L6-L10
    JournalMonthly Notices of the Royal Astronomical Society
    Issue number1
    Publication statusPublished - 1998


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