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

Details A radiation-driven disk wind model for massive young stellar objects A radiation-driven disk wind model for massive young stellar objects

1998-01-06

arxiv.org/abs/astro-ph/9801035v1

Astronomy and Astrophysics

Astrophysics

5 pages, LaTeX including one table, requires mn.sty, 4 Postscript figures, to appear in MNRAS as a Letter

Scientific paper

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 about 200 km/s 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.

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