On the Solar Differential Rotation: Meridional Motions Associated with a Slowly Varying Angular Velocity
Abstract
The paper calculates the meridional flow in the solar convection zone from the azimuthal momentum equation and compares the results with the existing surface observations. The dominant flows are found to contain only a few cells per hemisphere. Other than the meridional flow, the azimuthal momentum equation contains the velocity correlations (ur uphi) and (utheta uphi), as well as the angular velocity, Omega. The stream functions psi2 and psi4 define meridional motions with one and two latitudinal cells, respectively. The resultant meridional flow has a one-cell component rising at the equator and a two-cell component sinking at midlatitudes, in agreement with observations.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- April 1993
- DOI:
- 10.1086/172519
- Bibcode:
- 1993ApJ...407..367D
- Keywords:
-
- Angular Velocity;
- Meridional Flow;
- Solar Convection (Astronomy);
- Solar Physics;
- Solar Rotation;
- Solar Interior;
- Stream Functions (Fluids);
- Solar Physics;
- HYDRODYNAMICS;
- SUN: INTERIOR;
- SUN: ROTATION