Abstract
I present axisymmetric numerical simulations of the solar interior, with differential rotation imposed in the convection zone and tachocline and a dipolar poloidal field confined to the radiative interior. In these simulations toroidal field reversals which are equator-ward propagating are driven in the absence of a dynamo. These reversals are driven in the tachocline and are seen at the top of the convection zone. While not solar-like in many ways, these reversals do show some solar-like properties not previously seen in full MHD simulations.
| Original language | English (US) |
|---|---|
| Title of host publication | Proceedings of the International Astronomical Union |
| Pages | 62-68 |
| Number of pages | 7 |
| Volume | 6 |
| Edition | S271 |
| DOIs | |
| Publication status | Published - Jun 2010 |
Publication series
| Name | Proceedings of the International Astronomical Union |
|---|---|
| Number | S271 |
| Volume | 6 |
| ISSN (Print) | 17439213 |
| ISSN (Electronic) | 17439221 |
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Keywords
- Magnetic fields
- Sun: interior
ASJC Scopus subject areas
- Astronomy and Astrophysics
Cite this
Rogers, T. (2010). Toroidal field reversals. In Proceedings of the International Astronomical Union (S271 ed., Vol. 6, pp. 62-68). (Proceedings of the International Astronomical Union; Vol. 6, No. S271). https://doi.org/10.1017/S1743921311017455