3次元火星大気非静力学モデルの開発と鉛直対流の数値計算(宇宙・惑星(1),一般講演)

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  • Development of a three dimensional non-hydrostatic model for Martian atmosphere and a numerical simulation of thermal convection

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We develop a three dimensional non-hydrostatic model and perform a numerical simulation of thermal convection in the Martian atmosphere without background wind and dust radiative heating. The numerical model based on the two dimensional quasi-compressible model developed by Sugiyama et al. (2008). The atmospheric radiative transfer is not calculated explicitly, and a horizontally uniform body cooling is introduced below 5km height. After 12 hours of integration, the thermal convection whose horizontal scale of updraft region is several km is developed. The upward wind velocity reaches from 10 to 15m/sec while the downward wind velocity is about several m/sec. At the lowest level of the three dimensional model (z=50m), isolated vertical vortexes which horizontal scale is about several hundred m are developed frequently. This result suggests that the vertical vortex like dust devils may be naturally developed accompanied with the convective motion without background wind.

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