Feature description
Rapid rotation inhibits convection, however, this depends on the alignment of the rotation and gravity vectors. There's been previous work on formulating "rotating mixing-length theory" for parametrising convection. This does a very good job in the tropics/poles, but is not so well tested at the equator (due to numerical limitations).
Rapid rotation on early planets could readily inhibit convection in their atmospheres, impacting their cooling and mixing processes.
Preferred solution
It is trivial to incorporate the rotational effects of RMLT into the existing canonical MLT formalism in AGNI. This is described by eq 27 and 28 in Stevenson+78.
Also investigated more recently by this paper and this other paper.
Additional information
Feature description
Rapid rotation inhibits convection, however, this depends on the alignment of the rotation and gravity vectors. There's been previous work on formulating "rotating mixing-length theory" for parametrising convection. This does a very good job in the tropics/poles, but is not so well tested at the equator (due to numerical limitations).
Rapid rotation on early planets could readily inhibit convection in their atmospheres, impacting their cooling and mixing processes.
Preferred solution
It is trivial to incorporate the rotational effects of RMLT into the existing canonical MLT formalism in AGNI. This is described by eq 27 and 28 in Stevenson+78.
Also investigated more recently by this paper and this other paper.
Additional information