Planetary Origins and Development (OxPOD)

行星起源与发展（OxPOD）

• 批准号: ST/V000527/1
• 负责人: Hauke Marquardt
• 金额: $ 57万
• 依托单位: University of Oxford
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2021
• 资助国家: 英国
• 起止时间: 2021 至 无数据
• 项目状态: 未结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FV000527%2F1
• 关键词: Planetary; Origins; Development; OxPOD

Based on radioactive dating of the oldest particles in meteorites, the solar system formed from a flattened disk of gas and dust about 4.57 billion years ago. With the sun at the centre going through its earliest, violent stages of development, gases such as hydrogen, helium, water ammonia and methane were swept to the outermost parts, beyond the asteroid belt, where they were condensed into the giant planets Jupiter, Saturn, Uranus and Neptune. The inner solar system consisted predominantly of dust and this dust gradually clumped together over 10's of thousands of years and grew into a large number of bodies of 10-100 km in size. Over periods of 3 to 30 million years these small bodies collided and grew into the inner planets, Mercury, Venus, Earth and Mars, leaving the smaller asteroids of the asteroid belt as remnants of the period before the planets grew.This project is aimed at the understanding of some of the most important processes which took place on small asteroids and during growth of the planets using a combination of studies of meteorites and experiments aimed at simulating conditions on growing planets during the earliest history of the solar system. We are particularly interested in how the inner planets acquired their inventories of the so-called "moderately volatile elements" such as sulphur, chlorine, zinc and lead, and how these and other volatile elements, notably the noble gases Helium, Neon, Argon, Krypton and Xenon, are degassed to the atmosphere and recycled to the planet's interior. We are also building the capacity to simulate experimentally the conditions deep within the outer solar system planets Uranus and Neptune, which are believed to contain significant amount of methane. Individually our 5 inter-related projects may be summarised as follows:A. Addresses the question of how the planets of the inner solar system obtained their current concentrations of moderately volatile non-metals such as sulphur and chlorine and asks if the mechanisms of acquisition are different from those in which the volatile metals such as zinc, lead antimony and copper were acquired. This involves melting rocks containing these elements at temperatures of about 1300oC and determining the rates at which the different elements are lost to the atmosphere.B. What are the physical and chemical pathways by which sulphur is cycled through Io's interior? Io, a moon of Jupiter, is the most volcanically active body in the solar system and its atmosphere is being continually replenished by sulphur-rich gases emitted by volcanoes. This project uses computer modelling to address the ways in which sulphur is emitted to the atmosphere, condensed on the surface and then recycled to the interior.C. How has hydration of the martian surface led to recycling of volatiles including water, the noble gases, chlorine, bromine and iodine? These gases become fixed on Mars' surface by being locked into a common mineral, amphibole. The aim of this project is to determine, by high pressure experiment, the extents to which these elements can be trapped in amphibole and recycled to the martian interior.D. How did addition of water to carbon-rich asteroids lead to the growth of magnetite? A large proportion of carbonaceous meteorites have undergone aqueous alteration on their parent bodies and magnetite is an important clue to the processes involved. This project is aimed at experimentally simulating in the laboratory the transformation processes which lead to magnetite of the types observed.E. What are the properties of methane and water under the extreme pressure and temperature conditions in the interiors of Uranus and Neptune? This project is aimed at determining which compounds of methane and water are stable in the interiors of these giant planets and providing data to enable modelling of the planetary properties.

基于陨石中最古老的颗粒的放射性测年，太阳系由大约45.7亿年前的气体和灰尘呈扁平的磁盘形成。随着中心的太阳经历了其最早的发育范围，氢，氦气，水氨和甲烷等气体被扫到了小行星带外的最外部部分，在那里它们被凝结到巨型行星木星，土星，天王星，天王星和黑金河中。内部太阳系主要由灰尘组成，而这种灰尘逐渐凝结了10千年的时间，并成长为大量10-100 km的尸体。在超过3到3000万年的时间里，这些小物体碰撞并成长为内部行星，汞，维纳斯，地球和火星，使小行星带的较小小行星成为行星发展前的遗迹，该项目的旨在理解一些最重要的过程，这些过程是在小型小星际和逐步的过程中进行的，这些过程是在小星球上以及在集中阶段进行的，并且是在小星球上的成长中的一部分。在太阳系最早的历史上，生长的行星不断发展。我们对内在行星如何获取他们对所谓的“中度波动元素”（例如硫，氯，锌和铅）的清单，以及这些和其他挥发性元素如何脱离贵族氦气，霓虹灯，氩，氩，krypton和Xenon，都脱落到大气层和循环中。我们还建立了实验模拟天王星和海王星深处的条件的能力，据信它们含有大量的甲烷。单独地，我们的5个相互关联的项目可以总结如下：解决了内部太阳系的行星如何获得其当前挥发性非金属（例如硫和氯）的当前浓度的问题，并询问采集机制是否与获取锌金属（例如锌，铅氧合和铜）等挥发性金属的机制是否不同。这涉及在大约1300oC的温度下融化的岩石，并确定在大气中损失不同元素的速率。硫磺通过IO内部循环的物理和化学途径是什么？ IO是木星的月亮，是太阳系中最活跃的身体，它的气氛不断地被火山发出的富含硫的气体补充。该项目使用计算机建模来解决将硫发射到大气中的方式，在表面凝结，然后再回收到内部。火星表面的水合如何导致挥发物的回收利用，包括水，贵气体，氯，溴和碘？这些气体通过锁定在通用的矿物闪石中，将其固定在火星表面上。该项目的目的是通过高压实验来确定这些元素可以被困在闪石中并回收到火星内部的范围。在富含碳的小行星中加水如何导致磁铁矿的生长？很大一部分碳陨石对其母体进行了水性改变，而磁铁矿是所涉及过程的重要线索。该项目旨在在实验室中实验模拟转化过程，从而导致观察到的类型的磁铁矿。e。天王星和海王星内部的极端压力和温度条件下甲烷和水的特性是什么？该项目旨在确定这些巨型行星的内部甲烷和水的哪种化合物稳定，并提供数据以实现行星特性的建模。

项目成果

A MHz X-ray diffraction set-up for dynamic compression experiments in the diamond anvil cell.

• DOI: 10.1107/s1600577523003910
• 发表时间: 2023-07-01
• 期刊: Journal of synchrotron radiation
• 影响因子: 2.5

MHz free electron laser x-ray diffraction and modeling of pulsed laser heated diamond anvil cell

• DOI: 10.1063/5.0149836
• 发表时间: 2023-09
• 期刊: Journal of Applied Physics
• 影响因子: 3.2
• 作者: N. Jaisle;David Cébron;Z. Konôpková;R. Husband;C. Prescher;V. Cerantola;A. Dwivedi;J. Kaa;K. Appel;K. Buakor;O. B. Ball;R. S. McWilliams;C. Strohm;M. Nakatsutsumi;U. Zastrau;C. Baehtz;Marzena Anna Baron;E. Edmund;Joydipa Biswas;J. D. McHardy;B. Sturtevant;L. Ehm;Alexander F. Goncharov;M. McMahon;J. Buchen;H. Cynn;E. J. Pace;H. Liermann;D. Sneed;Samantha C. Cooper;Madison Anae;Jaeyong Kim;Zhongyan Wu;Yongjae Lee;H. Hwang;Taehyun Kim;Jinhyuk Choi;Jeongmin Lee;S. Merkel;J. Chantel;E. Koemets;H. Marquardt;V. Prakapenka;S. Chariton;Elena Shevchenko;G. Fiquet;A. Rosa;M. Mezouar;G. Garbarino;G. Morard

A MHz X-ray diffraction set-up for dynamic compression experiments in the diamond anvil cell

用于金刚石砧室动态压缩实验的 MHz X 射线衍射装置

• DOI: 10.3204/pubdb-2023-03846
• 发表时间: 2023
• 作者: Husband R