Observable Effects of B fields on the Winds and Envelopes of Hot Stars
| dc.creator | Cassinelli, Joseph P. | |
| dc.date | 2001-06-06 | |
| dc.date.accessioned | 2026-07-07T01:58:50Z | |
| dc.date.available | 2026-07-07T01:58:50Z | |
| dc.description | Magnetic fields on hot stars can produce a variety of interesting effects on the velocity, density, and temperature structure in the winds from the stars. The fields can produce a longitudinal dependence of the mass flux, which would lead to cyclical variability such as that seen in optical and UV spectra of many early-type stars. The fields can channel and spin-up the outflow, which appears to be needed to explain the disk-like density enhancements around Ap and Be stars. Magnetic confinement of hot gases can occur and be responsible for the anomalously high EUV fluxes seen in B giants, and the anomalous high ion X-ray line emission that is seen in recent CHANDRA observations. Special attention is given to the reports at this meeting that A stars develop magnetic Ap phenomenon only after about 30 percent of their main sequence lifetimes. A similar delay occurs for the emission line Be stars. It is suggested that these delays are related to the time it takes for fields to rise through the sub-adiabatic envelope to the surface starting from the interface between the convective-core and radiative-envelope where they are generated. | |
| dc.description | To appear in: Magnetic Fields Across the Hertzsprung-Russell Diagram, ASP Conf. Series | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0106116 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0106116 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/2873 | |
| dc.subject | Astrophysics | |
| dc.title | Observable Effects of B fields on the Winds and Envelopes of Hot Stars | |
| dc.type | text |