Theoretical and numerical study on Jovian atmospheres:their dynamics, matetialtrensport, and energetics.

为了研究木星行星大气的动力学、热学和成分结构之间的相互作用，我们汇编了相关知识的现状，开发了一个分层模拟系统，并用这些分层模拟系统进行了数值实验。我们的主要研究成果总结如下：1.我们发展了一个垂直的一维平衡云凝结模式，它使我们能够覆盖木星行星可能的大气成分变化。我们发现，与H_2O相比，与NH_3凝结和NH_4SH形成有关的云层对稳定性强度的贡献是不可忽略的。我们发展了一个包含NH_3和H_2O凝结和NH_4SH形成的二维云对流模式。我们进行了一系列的数值实验，发现H2O凝聚能级是一个明显的动力学…将上方和下方的对流运动分开的更多边界。NH3和NH4SH云的稳定层不能抑制H2O凝结愈合所驱动的云羽，导致H2O凝结层以上大气全深度的混合。考虑到木星大气的应用，我们用三维Bousinesq球壳对流模式对赤道加速度进行了一系列的数值研究。我们发现，外层有一个较强的稳定层有助于赤道逆行急流的发展。这一结果可能会提出一个关于旋转球面热对流解释木星和土星赤道西风急流原因的理论问题。开发了一个通用的软件基础设施，在此基础上构建了这些数值模型。它包含“gt4f90io”和“rdoc”，前者是一个用于数值数据I/O的库，后者是一个用于数值模型代码的自动文档生成器。我们还组织了一个标准风格的Fortran 90程序设计，并建立了一个用于基本数学操作的Fortran 90函数库，我们用它开发了一组谱模型。所有提到的软件都在我们的网站上向公众开放。

For the purpose of investigating the interplay among dynamical, thermal, and compositional structures of the atmospheres of Jovian planets, we compiled the current status of corresponding knowledge, developed a hierarchical modeling system, and conducted numerical experiments with those hierardical modeling systems. The main findings of our investigations are summarized as follows:1. We developed a vertical one-dimensional equilibrium cloud condensation model, which enable us to cover possible atmospheric compositional varieties of the Jovian planets. We found that the contributions to the intensity of stability by the cloud layers associated with the condensation of NH_3 and formation of NH_4SH are not negligible compared with that of H_2O.2. We developed a two-dimensional cloud convection model incorporating the condensation of NH_3 and H_2O and formation of NH_4SH. We conducted a series of numerical experiments, and found that the H_2O condensation level acts as a distinct dynamical … More boundary that separates the convective motions above and below it. The stable layers due to NH_3 and NH_4SH clouds cannot suppress the cloudy plumes driven by H_2O condensation healing, resulting in the mixing over the full depth of the atmosphere above the H_2O condensation level.3. With the application to the Jovian atmosphere in mind, we performed a series of numerical studies on the equatorial acceleration using the three dimensional Bousinesq spherical shell convection model. We found that a strong stable layer in the outer layer helps the development of equatorial retrograde jet. This result may raise a question about the theory where rotating spherical thermal convection explains the cause of the equatorial westerly jets of Jupiter and Saturn.4. A common software infrastructure, over which those numerical models were constructed, was developed. It contains "gt4f90io" which is a library for I/O of numerical data, and "Rdoc" which is an automatic documentation generator for numerical model codes. We also organized a standard style of Fortran90 programming and constructed a library of Fortran90 functions for basic mathematical manipulations, with which we developed 'Spmodel" which is a set of spectral models. All of the softwares mentioned are open to public on our web site. Less