A Magnetic Rotator Wind Disk Model for Be Stars
| dc.creator | Maheswaran, M. | |
| dc.date | 2004-09-29 | |
| dc.date.accessioned | 2026-07-07T02:14:48Z | |
| dc.date.available | 2026-07-07T02:14:48Z | |
| dc.description | A Magnetic Rotator Wind-Disk(MRWD) model is considered for the formation of Keplerian disks around Be stars. Material from low latitudes of the stellar surface flows along magnetic flux tubes and passes through a shock surface to form a pre-Keplerian disk region. Initially, the density in this region is small. After a fill-up time, the density of the disk is significantly larger and the magnetic force becomes negligible compared with the centrifugal force. The material then expands to form a Keplerian disk. During disk fill-up, the meridional component B-star of the magnetic field at the stellar surface must be larger than a minimum value B-star-min. The radial extent of the Keplerian region will be larger when B-star is larger or when viscosity plays a role. In B-type stars, B-star-min must be of order 1 G to 10 G. In faster rotating stars, the wind speed must be correspondingly larger for the formation of shock-compressed disk regions. | |
| dc.description | 5 pages, 2 figures. Submitted to ASP Conf. Ser. on "The Nature and Evolution of Disks Around Hot Stars", eds.: R. Ignace & K. Gayley | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0409738 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0409738 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/8268 | |
| dc.subject | Astrophysics | |
| dc.title | A Magnetic Rotator Wind Disk Model for Be Stars | |
| dc.type | text |