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

Janet E. Drew, Daniel Proga, James McLellan Stone

Research output: Contribution to journalArticle

38 Scopus citations

Abstract

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.

Original languageEnglish (US)
Pages (from-to)L6-L10
JournalMonthly Notices of the Royal Astronomical Society
Volume296
Issue number1
DOIs
StatePublished - May 1 1998

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Accretion, accretion discs
  • Circumstellar matter
  • Hydrodynamics
  • Methods: numerical
  • Stars: mass-loss
  • Stars: pre-main-sequence

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