Defining the thermal environment of the proto-planetary circumsolar disk: Continuation

定义原行星环日盘的热环境：续

• 批准号: ST/G002029/1
• 负责人: Philip Bland
• 金额: $ 25.31万
• 依托单位: Imperial College London
• 依托单位国家: 英国
• 项目类别: Research Grant
• 财政年份: 2010
• 资助国家: 英国
• 起止时间: 2010 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FG002029%2F1
• 关键词: Defining; thermal; environment; proto; planetary

What were conditions like when the planets were being formed, and what were the major factors that affected their formation? What was the solar system made from? How likely is it that similar processes acted to form planets such as the Earth and Mars around other stars? What can we learn about the possible existence of terrestrial-type planets elsewhere in the galaxy from studying the origins of our own planetary system? These are a few of the questions that we hope to help answer in the proposed research. It is thought that the solar system was formed from a nebula - a cloud of dust and gas. The composition of that material is not known, but we do know that a section of the nebula collapsed under gravity, formed a disk around the young Sun (a so-called proto-planetary disk), and underwent processing at a range of temperatures, in a wide variety of environments, before clumping together to make planets. We're lucky in having a collection of samples that date from this earliest period in solar system history. Primitive meteorites are amongst our only samples of the proto-planetary nebula. In the most primitive meteorites, the mineralogy and chemistry of this material suggests that it escaped subsequent thermal and aqueous alteration within the asteroid. As such, it offers a unique window on conditions in the disk prior to accretion of the first solids. Our knowledge of the thermal environment of the early solar system comes from chemical and mineralogical analyses of these rare meteorites. But those models are largely based on the chemistry of large (a few grams) of bulk heterogeneous meteorites, where components formed in very different environments are measured together. Over recent years, our group has been at the forefront of extending the boundaries of cosmochemistry, using new tools to unravel early solar system processes. We have developed a unique methodology that allows us to determine the chemistry of some of the earliest solids formed in the inner solar system. We have proven the effectiveness of our technique, and our preliminary data already challenge existing models. We are world leaders in this type of work, and are now able to define the compositional makeup for individual components within these highly heterogeneous objects, for the first time. Knowing the chemistry of chondritic components allows us to define the thermal environment of our own proto-planetary disk - its heterogeniety, as well as processes such as volatile depletion (the mechanism by which we arrived at rocky inner planets, as opposed to objects like Uranus), and chondrule formation (the mechanism by which some of the first solids were formed). Understanding the chemistry and thermal environment of our own proto-planetary disk is vital in understanding its formation and evolution, and more generally, how disks and planets around other stars may have formed. Our proposal is for two years funding for a postdoctoral research scientist - an individual who is already a specialist in the relevant techniques - in addition to funding to cover instrumentation costs and consumables. The research is specifically relevant to the theme of 'How do planetary systems evolve', and 'How were the chemical elements created', outlined in the STFC Delivery Plan 2008/9-2011/12.

行星形成时的条件是什么，以及影响其形成的主要因素是什么？太阳系是由什么制造的？类似的过程以形成其他恒星周围的地球和火星等行星的可能性有多大？我们可以从研究我们自己的行星系统的起源来了解什么了解银河系其他地方的陆地型星球的可能存在？这些是我们希望在拟议的研究中帮助回答的一些问题。人们认为太阳系是由星云形成的 - 灰尘和气体云。该材料的组成尚不清楚，但我们确实知道，在重力下崩溃的一部分在重力下崩溃了，在年轻的太阳周围形成了一个圆盘（一个所谓的原始星际磁盘），并在各种环境中进行了多种温度的处理，然后在各种环境中进行处理，然后再团结起来制造行星。我们很幸运能收集一系列可追溯到太阳系历史上最早时期的样品。原始陨石是我们原始星云的唯一样品之一。在最原始的陨石中，该材料的矿物学和化学表明它逃脱了小行星内随后的热和水性改变。因此，它为磁盘中的条件提供了独特的窗口，然后再增加第一固体。我们对早期太阳系热环境的了解来自对这些稀有陨石的化学和矿物学分析。但是这些模型主要基于大型（几克）散装异质陨石的化学性质，在这些陨石中，在非常不同的环境中形成的成分被一起测量。近年来，我们的小组一直处于扩展宇宙化学界限的最前沿，并使用新工具来解开早期太阳系过程。我们开发了一种独特的方法，使我们能够确定内部太阳系中一些最早的固体的化学性质。我们已经证明了技术的有效性，并且我们的初步数据已经挑战了现有模型。我们是这类工作中的世界领导者，现在能够首次为这些高度异构物体内的各个组件定义组成构成。了解软骨成分的化学性能使我们能够定义自己的原始星际磁盘的热环境 - 其异质酶以及诸如挥发性消耗之类的过程（我们到达岩石内行星的机制，与诸如wryanus之类的物体相反）和小节形成（构成了某些固体构成的物体）。了解我们自己的原始星际磁盘的化学和热环境对于理解其形成和进化至关重要，更普遍地，其他恒星周围的磁盘和行星可能形成。我们的建议是两年的资金，用于博士后研究科学家（一个已经是相关技术专家的人），此外还可以资助仪器成本和消耗品。这项研究与“行星系统如何发展”和“化学元素如何创建”的主题特别相关，该主题是STFC交付计划2008/9-2011/12中概述的。

项目成果

Earliest rock fabric formed in the Solar System preserved in a chondrule rim

• DOI: 10.1038/ngeo1120
• 发表时间: 2011-04-01
• 期刊: NATURE GEOSCIENCE
• 影响因子: 18.3
• 作者: Bland, Philip A.;Howard, Lauren E.;Dyl, Kathryn A.
• 通讯作者: Dyl, Kathryn A.