JpGU-AGU Joint Meeting 2020

Presentation information

[J] Oral

M (Multidisciplinary and Interdisciplinary) » M-IS Intersection

[M-IS27] Geophysical fluid dynamics-Transfield approach to geoscience

convener:Keita Iga(Atmosphere and Ocean Research Institute, The University of Tokyo), Shigeo Yoshida(Department of Earth and Planetary Sciences, Faculty of Sciences, Kyushu University), Takatoshi Yanagisawa(Research Institute for Marine Geodynamics, Japan Agency for Marine-Earth Science and Technology), Hidenori AIKI(Nagoya University)

[MIS27-05] Equatorial superrotation due to heating and cooling in a 1-1/2 layer shallow water system.

*Rin Fujibayashi1, Hiroki Kashimura1, Yoshiyuki O. Takahashi1, Yoshi-Yuki Hayashi1 (1.Department of Planetology, Graduate School of Science, Kobe University)


On Venus, Titan and tidally locked exoplanets, a wind blows at the equator in the direction of their planetary rotation. Such zonal wind is called “superrotation”. Showman and Polvani (2010) showed that equatorial superrotation can be generated in the presence of heating and cooling in a 1-1/2 layer shallow-water model that consists of an active upper layer and a deep, quiescent lower layer and includes vertical advection of planetary momentum from the lower layer to the upper layer. They showed a result with a time constant for drag τdrag = 5 days, a radiative time constant τrad = 5 days, and Earth-like values for other planetary parameters; however parametric dependence of the superrotation was not explored. In this study, we perform parameter experiments in which the drag time constant is varied from 0.1 days to infinity.

In our numerical experiments, equatorial superrotation is generated in all cases, and the equatorial zonal-mean zonal flow ū becomes faster as the drag time constant increases. The increasing rate of ū with respect to τdrag is ū ∝ τdrag2 when τdrag ≦ 1 day; whereas that decreases as τdrag increases when τdrag > 1 day.

Momentum balance analyses reveal that an eastward acceleration by the meridional flux convergence of the zonal eddy momentum is nearly canceled by a westward acceleration due to forcing to the mass. This means that the acceleration caused by the planetary momentum advection from the lower layer to the upper layer, expressed by the term R, is important for generation and maintenance of the superrotation. If the acceleration does not depend on the drag time constant, then it is expected that ū ∝ τdrag1 from the balance between the term R and the Rayleigh friction due to the zonal-mean zonal flow. However, our numerical results show that the relationship between the equatorial zonal-mean zonal flow and the drag time constant is not in the simple proportional relationship.

When the drag time constant is short as τdrag ≦ 1 day, the balance between the pressure gradient due to height disturbances and the friction by flow disturbances is dominant. Therefore, the magnitude of the flow disturbances increases in proportional to the drag time constant. In addition, the term R is in proportional to the magnitude of the flow disturbances. Hence, ū seems to be in proportional to τdrag2. On the other hand, when the drag time constant is long as 1 < τdrag ≦ 50 days, the westerly flow in the heating region (Q > 0) grows as τdrag increases but easterly flow there hardly changes (in our numerical results). As a result, the term R decreases and the increasing rate of ū decreases as the drag time constant increases. Finally, when the drag time constant is very long as τdrag > 50 days, numerical solutions do not achieve steady states and are not similar to the Matsuno-Gill pattern. In addition, an instability occurs, which may affect the generation and maintenance of the equatorial superrotation.