Planetary Science at the Open University 2017-2020

我们拟议的研究方案涉及太阳系的起源和演变，包括类地行星、月球、小行星、彗星、冰卫星和地外物质的表面、大气层和物理、地质、化学和生物过程，这些项目涉及科学技术委员会科学路线图挑战B：“恒星和行星系统如何发展，生命是我们星球独有的吗？“太阳系内部的岩石天体在理解行星系统演化方面特别重要，因为它们有着共同的起源，但随后的历史却各不相同。月球样品将用于确定月球上挥发性元素的丰度和组成，它们在月球内部的来源，以及影响它们在月球地质历史中演变的过程。氧同位素分析将用于确定太阳系形成的最早阶段形成物质的条件和过程。火星是国际太阳系探索方案的重点，最终目标是火星样品返回。我们将：通过综合大气模型、空间使命数据和表面地质学，在全球和局部尺度上调查火星水循环;通过测量不同年代的火星陨石中捕获的示踪剂，评估火星大气成分随时间的潜在变化;确定二氧化碳而不是水流是否能够解释火星最近活跃的表面特征。水星是行星形成光谱中的一个末端成员，我们计划利用NASA信使号的数据来研究它的起源和地壳演化，并为欧空局的BepiColombo使命做准备。太阳系的寒冷外部区域，特别是彗星，被认为保留了一些最原始的原始物质。我们计划探索彗星物质的组成和起源，并通过以下方式了解驱动彗星活动的过程：对最原始的行星际尘埃颗粒进行实验室分析;通过罗塞塔使命上的仪器直接测量彗星，以及实验室模拟。我们将对辐照冰进行实验室紫外线观测，以提供对太阳系冰的组成以及它们如何在母体周围创造大气的新见解。我们还将研究挥发物在太阳系小天体的凝聚（“制造”）中所起的作用，以及通过热循环（一种“打破”它们的候选过程）所能实现的碎裂。地球是否是太阳系中生命的独特位置的问题仍然是我们这个时代最持久的问题之一。我们计划研究如果存在生命，火星，欧罗巴和土卫二上潜在的可居住环境的地球化学将如何在地质时间尺度上发生变化，从而产生可用作太阳系生命证据的可区分的生物标志物。我们将研究超高速撞击在以下方面的作用：处理对可居住性至关重要的化合物（水、硫物质、有机物质）;以及加拿大直径100公里的Manicouagan撞击结构的热液系统，以评估早期火星热液系统的天体生物学意义。除了满足人类探索和了解周围宇宙的先天愿望外，对我们来说，我们的研究有更多实实在在的好处。我们将空间和实验室仪器开发所涉及的分析技术应用于医药、安全、旅游和化妆品等不同领域的公司。我们的研究的最重要的好处之一是，它有助于培养和激励学生-下一代的科学家和工程师-通过大学内的培训和公共宣传和学校计划。

Our proposed research programme addresses the origin and evolution of the Solar System, including surfaces, atmospheres and physical, geological, chemical and biological processes on the terrestrial planets, the Moon, asteroids, comets, icy satellites and extraterrestrial materials, in a range of projects which address the STFC Science Roadmap challenge B: "How do stars and planetary systems develop and is life unique to our planet?"The inner rocky bodies of the Solar System are of particular importance in understanding planetary system evolution, because of their common origin but subsequent divergent histories. Lunar samples will be used to determine the abundance and composition of volatile elements on the Moon, their source(s) in the lunar interior, and processes influencing their evolution over lunar geological history. Oxygen isotope analysis will be used to determine the conditions and processes that shape the formation of materials during the earliest stages of Solar System formation. Mars is the focus of international Solar System exploration programmes, with the ultimate aim of Mars Sample Return. We will: investigate the martian water cycle on global and local scales through a synthesis of atmospheric modeling, space mission data and surface geology; assess potential changes in the composition of Mars' atmosphere over time through measurement of tracers trapped in martian meteorites of different ages; and determine whether carbon dioxide, rather than water flow, is able to account for recently active surface features on Mars. Mercury is an end-member in the planet-formation spectrum and we plan to exploit NASA MESSENGER data to study its origin and crustal evolution, and prepare for ESA's BepiColombo mission.The cold outer regions of the Solar System, and particularly comets, are believed to have retained some of the most pristine primitive material from their formation. We plan to probe the composition and origins of cometary material and understand the processes that drive cometary activity through: laboratory analysis of the most primitive Interplanetary Dust Particles; and direct measurements of a comet by our instruments on the Rosetta mission, together with laboratory simulations. We will conduct laboratory ultraviolet observations of irradiated ices to provide new insights into the composition of Solar System ices and how they may create atmospheres around their parent bodies. We will also investigate the role volatiles can play in the cohesion ("making") of Solar System minor bodies, and the fragmentation that can be achieved by thermal cycling (a candidate process that "breaks" them).The question of whether Earth is a unique location for life in the Solar System remains one of the most enduring questions of our time. We plan to investigate how the geochemistry of potentially habitable environments on Mars, Europa and Enceladus would change over geological timescales if life was present, producing distinguishable biomarkers that could be used as evidence of life in the Solar System. We will study the role of hypervelocity impacts in: the processing of compounds of critical interest to habitability (water, sulfur-species, organic species) during crater formation; and the hydrothermal system of the 100 km diameter Manicouagan impact structure in Canada to assess the astrobiological implications of hydrothermal systems for early Mars.In addition to satisfying humanity's innate desire to explore and understand the Universe around us, our research has more tangible benefits. We use the analytical techniques involved from development of space and laboratory instrumentation for applications with companies in fields as diverse as medicine, security, tourism and cosmetics. One of the most important benefits of our research is that it helps to train and inspire students - the next generation of scientists and engineers - through training within the University and public outreach and schools programmes.