A two-layer $αω$ dynamo model, and its implications for 1-D dynamos
| dc.creator | Roald, Colin B. | |
| dc.date | 1999-04-27 | |
| dc.date.accessioned | 2026-07-07T02:31:24Z | |
| dc.date.available | 2026-07-07T02:31:24Z | |
| dc.description | I will discuss an attempt at representing an interface dynamo in a simplified, essentially 1D framework. The operation of the dynamo is broken up into two 1D layers, one containing the $α$ effect and the other containing the $ω$ effect, and these two layers are allowed to communicate with each other by the simplest possible representation of diffusion, an analogue of Newton's law of cooling. Dynamical back-reaction of the magnetic field on $ω$ is included. I will show extensive bifurcation diagrams, and contrast them with diagrams I computed for a comparable purely 1D model. The bifurcation structure shows remarkable similarity, but a couple of subtle changes imply dramatically different physical behaviour for the model. In particular, the solar-like dynamo mode found in the 1-layer model is not stable in the 2-layer version; instead there is an (apparent) homoclinic bifurcation and a sequence of periodic, quasiperiodic, and chaotic modes. I argue that the fragility of these models makes them effectively useless as predictors or interpreters of more complex dynamos. | |
| dc.description | paper presented at the Workshop on Stellar Dynamos: Chaotic flows and nonlinearities (8 pp, 5 figures) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9904369 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9904369 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/14142 | |
| dc.subject | Astrophysics | |
| dc.title | A two-layer $αω$ dynamo model, and its implications for 1-D dynamos | |
| dc.type | text |