Atmospheric modelling of tidally-locked exoplanets

气候模型使我们能够研究地球系统的控制过程、动力学和局限性，包括能够彻底改变气候的反馈。这些模型也被用来研究其他行星气候的多样性，特别是可能导致生命出现的宜居条件的范围。最丰富的潜在宜居行星群是那些绕M矮星运行的行星，詹姆斯韦伯太空望远镜（JWST）最近的发射和技术进步将有助于进一步的研究。初步的模拟研究表明，这些行星的大气层可能是稳定的，尽管它们具有潮汐锁定的性质，尽管有一个不寻常的气候学，这可能对它们的可居住性产生影响。利用现有的大量地球气候数据，该项目将开始探索基于气候学的地表适居性定义。具体而言，该定义应能够应用于3D气候模型输出数据，并允许比较具有不同轨道特性的各种行星和恒星宿主之间的可居住性。随后将对表面可居住性的“概括”进行调查，即确定系外行星气候建模研究中常用的“水行星简化”是否提供了足够的近似值，以代表类地行星的气候和可居住性，一些未知的大陆配置。最后一章的重点是潮汐锁定行星的可居住性，旨在连接大气动力学与表面可居住性的空间格局，并建立在文献建立了行星自转周期与大气环流制度的依赖。

Climate models have enabled us to examine the governing processes, dynamics, and lim- its of the Earth system, including of the feedbacks that can drastically transform the climate. These models have also been adapted to study the diversity of other planetary climatologies, and in particular of the range of habitable conditions that might lead to the emergence of life. The most abundant group of potentially habitable planets are those orbiting M-dwarf stars, of which the recent launch and technological advances of the James Webb Space Telescope (JWST) will aid further investigation. Preliminary modelling studies have shown that the at- mospheres of these planets may be stable despite their tidally-locked nature, albeit with an unusual climatology which may have implications on their habitability. Making use of the plethora of Earth climate data available, the project will begin by exploring a climatologically- based definition of surface habitability. Specifically, this definition should have the ability to be applied to 3D climate model output data, as well as allow a comparison of habitability be- tween a diverse range of planets with different orbital properties and stellar hosts. This will be followed by an investigation into the 'generalisation' of surface habitability, that is, determin- ing whether the 'aquaplanet simplification' commonly used in exoplanet climate modelling studies provides an adequate approximation in representing the climate and habitability of an Earth-like planet some unknown continental configuration. The final chapter focuses upon the habitability of tidally-locked planets, aiming to connect the atmospheric dynamics with spatial patterns of surface habitability, and building upon the literature which establishes a dependence of planetary rotation period with atmospheric circulation regime.