The case for a distributed solar dynamo shaped by near-surface shear
| dc.creator | Brandenburg, Axel | |
| dc.date | 2005-02-15 | |
| dc.date.accessioned | 2026-07-07T02:16:59Z | |
| dc.date.available | 2026-07-07T02:16:59Z | |
| dc.description | Arguments for and against the widely accepted picture of a solar dynamo being seated in the tachocline are reviewed and alternative ideas concerning dynamos operating in the bulk of the convection zone, or perhaps even in the near-surface shear layer, are discussed. Based on the angular velocities of magnetic tracers it is argued that the observations are compatible with a distributed dynamo that may be strongly shaped by the near-surface shear layer. Direct simulations of dynamo action in a slab with turbulence and shear are presented to discuss filling factor and tilt angles of bipolar regions in such a model. | |
| dc.description | 10 pages, 6 figures, Astrophys. J. 625 (scheduled for the 1 June 2005 issue) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0502275 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0502275 | |
| dc.identifier | Astrophys.J. 625 (2005) 539-547 | |
| dc.identifier | doi:10.1086/429584 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/9005 | |
| dc.subject | Astrophysics | |
| dc.title | The case for a distributed solar dynamo shaped by near-surface shear | |
| dc.type | text |