[PPS04-P03] A Three-dimensional Numerical Simulation of Venus' Cloud-level Convection
Keywords:planetary atmosphere, numerical modeling
We use the convection resolving model developed by Sugiyama et al. (2009). The model is based on the quasi-compressible system (Klemp and Wilhelmson, 1978), and is used in the simulations of the atmospheric convections of Jupiter (Sugiyama et al., 2011, 2014) and Mars (Yamashita et al. 2017). We perform two experiments. The first one, which we call Ext.B, is based on Baker et al. (1998). A constant turbulent mixing coefficient is used in the whole computational domain, and a constant heat flux is given at the upper and lower boundaries as a substitute for radiative forcing. The second one, which we call Exp.I, is based on Imamura et al. (2014). The sub-grid turbulence process is implemented by Klemp and Wilhelmson (1989), and an infrared heating profile obtained in a radiative-convective equilibrium calculation (Ikeda, 2011) is used. In both of the experiments, the temporally averaged solar heating profile is used. The spatial resolution is 200 m in the horizontal direction and 125 m in the vertical direction. The domain covers 128 km x 128 km horizontally and altitudes from 40 km to 60 km. The horizontal domain size is set to be larger than that employed in Lefevre et al (2017) in order to permit the excitation of larger scale gravity waves.
In our poster, we will discuss the difference of convective motions and heat budgets obtained in Exp.B and Exp.I. We will also show the propagation of gravity wave driven by convection.