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

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

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.296l...6d&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 296, Issue 1, pp. L6-l10.

Astronomy and Astrophysics

Astronomy

41

Accretion, Accretion Discs, Hydrodynamics, Methods: Numerical, Circumstellar Matter, Stars: Mass-Loss, Stars: Pre-Main-Sequence

Scientific paper

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.

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