[MGI40-04] Dust lifting and advection simulated by a non-hydrostatic general circulation model in a Mars-like atmosphere
Keywords:Martian atmosphere, global simulation, non-hydrostati model
We are developing a non-hydrostatic global Martian atmospheric model (Martian SCALE-GM) which is suitable for large-scale parallel computation, targeting to perform high-resolution simulations described above on the supercomputer Fugaku. SCALE-GM (http://r-ccs-climate.riken.jp/scale/) is being developed by using the dynamical core of NICAM (Tomita and Satoh, 2005; Satoh et al., 2008; Satoh et al., 2014), a non-hydrostatic model using a finite volume method in the icosahedral grid systems (Tomita et al., 2001, 2002), that has been used for simulations of Earth atmosphere and climate, and by aiming at sharing of physical process modules with the regional model (SCALE-RM) and application to other planetary atmospheres. We are developing Martian SCALE-GM by incorporating constants and physical process modules of the Martian atmosphere. The Martian physical modules are taken from DCPAM (https://www.gfd-dennou.org/library/dcpam/), an existing pan-planetary atmospheric general circulation model (GCM). DCPAM is a traditional, hydrostatic GCM using a spectral method for horizontal discretization.
We have ported a Martian atmospheric radiation model (partially, Forget et al., 1999) and a soil model from DCPAM to SCALE-GM and performed a high-resolution calculation with 1.9 km grid-intervals by following settings. The atmosphere model has 36 layers, and distribution of dust is fixed with 0.2 optical depth. The soil model has 18 layers. Soil's heat capacity and thermal conductivity are set to 9.7×105 [J K−1 kg−1] and 0.076 [W m–1 K–1], respectively. Surface albedo is fixed at 0.5. For the calculation of surface fluxes and vertical diffusion, BH91B95 (Beljaars & Holstang, 1991; Beljaars, 1995) and MY2.5 (Mellor & Yamada, 1982) are used, respectively. The initial condition is the 200 K constant temperature atmosphere and soil. Note that a high albedo was used and the topography and the moist processes were not included in the above calculation.
In this study, we introduced a parameterization of dust lifting (Kahre et al., 2006) and the gravity sedimentation process (Lin & Rood, 1996) to the Martian SCALE-GM, and enable it to calculate dust processes of lifting, advection, and sedimentation. First we aimed to explore effects of the vertical convection and associated large surface stress that are expressed by non-hydrostatic high-resolition model to dynamical processes of the dust. We performed calculation with radiatively inactive dust (i.e., radiation do not depend on the dust distribution). The figure shows zonal-mean distribution of dust's mixing rate and the lifting rate averaged over 5 days after 26-day time-integration from the initial state, for horizontal grid-intervals of dx = 60 km, 30 km, and 15 km. A large amount of dust reaches high altitudes (upper panels) in the higher-resolution case. This can be because of the higher dust-lifting rate (lower panels) and more active vertical convection in the higher-resolution case. In our presentation, we will show and discuss the results of calculations with radiatively active dust too.