The truncation of stellar discs. A theoretical model
| dc.creator | Battaner, E. | |
| dc.creator | Florido, E. | |
| dc.creator | Jimenez-Vicente, J. | |
| dc.date | 1998-01-27 | |
| dc.date.accessioned | 2026-07-07T02:25:55Z | |
| dc.date.available | 2026-07-07T02:25:55Z | |
| dc.description | The truncation of stellar discs is not abrupt but characterized by a continuous distancing from the exponential profile. There exists a truncation curve, $t(r)$, ending at a truncation radius, $r_t$. We present here a theoretical model in which it is assumed that the magnetic hypothesis explaining the flat rotation curve also explains the truncation. Once stars are born, the centripetal magnetic force previously acting on the progenitor gas cloud is suddenly interrupted, and stars must move to larger orbits or escape. The agreement between theoretical and observed truncation curves is very satisfactory. Parameters defining the disc gas rotation curve should therefore be related to those defining the truncation. It is predicted that rotation curves that quickly reach the asymptotic value $θ_0 = θ(r=\infty)$ would have small truncation radii. On the contrary, $r_t$ and $θ_0$ itself, would be uncorrelated quantities. | |
| dc.description | 10 pages, 5 figures, LaTeX using A&A macros v4.. Also available as gzipped postscript at http://deneb.ugr.es/papers/trunky.ps.gz | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9801263 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9801263 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/12066 | |
| dc.subject | Astrophysics | |
| dc.title | The truncation of stellar discs. A theoretical model | |
| dc.type | text |