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 | |
| State | 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
Toroidal field reversals. / Rogers, Tamara.
Proceedings of the International Astronomical Union. Vol. 6 S271. ed. 2010. p. 62-68 (Proceedings of the International Astronomical Union; Vol. 6, No. S271).Research output: Chapter in Book/Report/Conference proceeding › Conference contribution
}
TY - GEN
T1 - Toroidal field reversals
AU - Rogers, Tamara
PY - 2010/6
Y1 - 2010/6
N2 - 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.
AB - 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.
KW - Magnetic fields
KW - Sun: interior
UR - http://www.scopus.com/inward/record.url?scp=84882781295&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84882781295&partnerID=8YFLogxK
U2 - 10.1017/S1743921311017455
DO - 10.1017/S1743921311017455
M3 - Conference contribution
AN - SCOPUS:84882781295
SN - 9780521197397
VL - 6
T3 - Proceedings of the International Astronomical Union
SP - 62
EP - 68
BT - Proceedings of the International Astronomical Union
ER -