A radiation-driven disk wind model for massive young stellar objects
| dc.creator | Drew, Janet E. | |
| dc.creator | Proga, Daniel | |
| dc.creator | Stone, James M. | |
| dc.date | 1998-01-06 | |
| dc.date.accessioned | 2026-07-07T02:25:44Z | |
| dc.date.available | 2026-07-07T02:25:44Z | |
| dc.description | 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. | |
| dc.description | 5 pages, LaTeX including one table, requires mn.sty, 4 Postscript figures, to appear in MNRAS as a Letter | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9801035 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9801035 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11990 | |
| dc.subject | Astrophysics | |
| dc.title | A radiation-driven disk wind model for massive young stellar objects | |
| dc.type | text |