Theories of rotating convection zones
Journal Article
·
· Astrophys. J.; (United States)
It is shown that the time rate of change brought about by turbulent convective motions in the angular momentum of a thin spherical shell is such as to increase the angular velocity of the lower part of the solar convection zone (SCZ) and to decrease the angular velocity of the upper part. Arguments are presented in favor of the following very tentative model of rotation in the SCZ: (1) the lower region is in weaker differential rotation than the surface and not constrained by the Taylor-Proudman theorem, and (2) the observed solar differential rotation at the surface is generated as the SCZ relaxes from the state in the lower part to the state at the surface. In the upper and lower layers of the SCZ, angular-momentum conservation between the turbulent motions and viscous stresses leads to an angular velocity increasing upward. 34 references.
- Research Organization:
- National Solar Observatory, Sunspot, NM
- OSTI ID:
- 5684470
- Journal Information:
- Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 297; ISSN ASJOA
- Country of Publication:
- United States
- Language:
- English
Similar Records
Behavior of the angular velocity in the lower part of the solar convection zone
MODELING OF DIFFERENTIAL ROTATION IN RAPIDLY ROTATING SOLAR-TYPE STARS
Numerical simulations of stellar convective dynamos. II. Field propagation in the convection zone
Journal Article
·
Tue Feb 28 23:00:00 EST 1989
· Astrophys. J.; (United States)
·
OSTI ID:6224965
MODELING OF DIFFERENTIAL ROTATION IN RAPIDLY ROTATING SOLAR-TYPE STARS
Journal Article
·
Mon Oct 10 00:00:00 EDT 2011
· Astrophysical Journal
·
OSTI ID:21587437
Numerical simulations of stellar convective dynamos. II. Field propagation in the convection zone
Journal Article
·
Sun Mar 31 23:00:00 EST 1985
· Astrophys. J.; (United States)
·
OSTI ID:5403652