Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2011-04-24
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
In press at ApJ. 20 pages, 12 figures. Animations can be found at http://www.solarphysicist.com
Scientific paper
We present axisymmetric simulations of the coupled convective and radiative regions in the Sun in order to investigate the angular momentum evolution of the radiative interior. Both hydrodynamic and magnetohydrodynamic models were run. We find an initial rapid adjustment in which the dif- ferential rotation of the convection zone viscously spreads into the radiative interior, thus forming a "tachocline". In polar regions the subsequent spread of the tachocline is halted by a counter-rotating meridional circulation cell which develops in the tachocline. Near the equator such a counter-rotating cell is more intermittent and the tachocline penetration depth continues to increase, albeit more slowly than previously predicted. In the magnetic models we impose a dipolar field initially confined to the radiative interior. The behavior of the magnetic models is very similar to their non-magnetic counter- parts. Despite being connected to the convection zone, very little angular momentum is transferred between the convective and radiative regions. Therefore, while it appears that a magnetic field is not necessary to stop the tachocline spread, it also does not promote such a spread if connected to the convection zone.
No associations
LandOfFree
On Limiting the Thickness of the Solar Tachocline does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with On Limiting the Thickness of the Solar Tachocline, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On Limiting the Thickness of the Solar Tachocline will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-544391