Planetary Origins and Development

行星起源与发展

• 批准号: ST/R000999/1
• 负责人: Bernard Wood
• 金额: $ 54.93万
• 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: 2018
• 资助国家: 英国
• 起止时间: 2018 至 无数据
• 项目状态: 已结题
• 来源: https://gtr.ukri.org/projects?ref=ST%2FR000999%2F1
• 关键词: Planetary; Origins; Development

Scientists can now detect Earth-sized planets orbiting other stars far away in our Milky Way galaxy. Yet, many basic aspects of how planets first form, then develop and function are unknown or surprisingly uncertain. The research in this proposal will address some of the questions to which scientists seek answers in this fascinating area. The subjects in which we work are called isotope cosmochemistry, petrology, rock physics and low temperature geochemistry. Four lead investigators with these different backgrounds will work together to address five big questions. 1. What processes generated the atoms from which our Solar System was built? Hydrogen and helium are mainly the product of the Big Bang 13.8 billion years ago. But what about all the heavier elements like calcium, titanium, chromium, nickel, zirconium, molybdenum or palladium? Since the 1950s there have been well accepted theories for how these heavier elements were synthesised in large stars. Now there is evidence these theories may be wrong. We will measure the proportions of the isotopes of these elements in some of the oldest material in the Solar System to test the new theories. 2. What processes govern the amount of volatile elements like tin in the terrestrial planets? We will perform experiments using a recently-built furnace to determine the relative losses and isotopic fractionation of such moderately volatile elements from molten asteroidal and planetary bodies. We will evaluate whether very early processes in the circumstellar disk were responsible or whether there were losses from large planetary volcanoes into space. This work may also tell us about the atmospheres of some hot exosolar planets. 3. How do metallic cores form and differentiate? The Earth like all terrestrial planets has an iron core. In the case of Earth it is partially liquid, so convects, generating a magnetic field. How do such cores form and then crystallise? We will measure isotopic variations in vanadium, chromium, nickel, molybdenum, palladium and tungsten in meteorites, which together with experiments, will provide new insights into core formation and crystallisation in early planetary embryos as well as larger objects. These are expected to also shed light on the nature of the Moon-forming impactor Theia.4. How do rocky planetary interiors respond to orbital stresses? On Earth we are aware of tidal forces from the Moon that cause the interior of a planet to move. Shortly after the Moon formed it was very close to Earth - it would have occupied a third of the night sky! So the tidal forces would have been vastly bigger. Yet we do not know much about how a rocky planet responds to such huge stresses. We will conduct laboratory experiments to evaluate this. 5. How do planetary crusts influence atmospheric evolution? One of the most important aspects of the development of habitable worlds is the formation of an atmosphere. However, the release of one of the most important and simple of elements, hydrogen, is not well understood. There are ideas emerging from climate modelling and origins of life studies that we will test with new experimental and modelling investigations of hydrogen generation through the interactions between water and rock.

现在，科学家可以在我们的银河系中检测到距离其他恒星的地球大小的行星。然而，行星首先形成，发展和功能的许多基本方面是未知或令人惊讶的不确定的。该提案中的研究将解决科学家在这个迷人地区寻求答案的一些问题。我们工作的受试者称为同位素宇宙化学，岩石学，岩石物理学和低温地球化学。具有这些不同背景的四名主要调查员将共同解决五个大问题。 1。哪些过程产生了我们的太阳系的原子？氢和氦主要是138亿年前大爆炸的产物。但是，所有较重的元素，例如钙，钛，铬，镍，锆，钼或钯呢？自1950年代以来，人们就这些较重的元素如何合成大恒星的理论。现在有证据表明这些理论可能是错误的。我们将在太阳系中一些最古老的材料中测量这些元素的同位素的比例，以测试新理论。 2.哪些过程控制着陆地行星中锡这样的挥发性元素的数量？我们将使用最近建造的熔炉进行实验，以确定从熔融小行星和行星体中这种中度挥发性元件的相对损失和同位素分馏。我们将评估Internelar磁盘中的非常早期的过程是负责的，还是大型行星火山进入太空的损失。这项工作还可以告诉我们一些热外星星球的气氛。 3。金属芯如何形成和区分？像所有陆地行星一样，地球都有铁芯。在地球的情况下，它是部分液体的，因此对流产生磁场。这样的核如何形成然后结晶？我们将测量钒，铬，镍，钼，钯和钨的同位素变化，这些变化将与实验一起提供新的见解，以对早期行星胚胎中的核心形成和结晶以及大物体提供新的见解。预计这些还可以阐明月球形成影响器Theia的性质4。岩石行星内饰如何应对轨道应力？在地球上，我们知道会导致行星内部移动的月球的潮汐力。月球形成后不久，它非常靠近地球 - 它将占据夜空的三分之一！因此，潮汐力量会更大。但是，我们对岩石星球如何应对如此巨大的压力并不了解。我们将进行实验室实验以评估这一点。 5。行星地壳如何影响大气进化？可居住世界发展的最重要方面之一是形成气氛。然而，释放最重要，最简单的元素之一，氢气，尚不清楚。我们将通过水与岩石之间的相互作用对生命研究的气候建模和生命研究的起源提出了一些想法。

项目成果

The effect of composition on chlorine solubility and behavior in silicate melts

成分对硅酸盐熔体中氯溶解度和行为的影响

• DOI: 10.2138/am-2022-8450
• 发表时间: 2023
• 期刊: Journal of Earth and Planetary Materials
• 作者: Thomas R

Sulfur oxidation state and solubility in silicate melts

硫的氧化态和在硅酸盐熔体中的溶解度

• DOI: 10.1007/s00410-023-02033-9
• 发表时间: 2023
• 期刊: Contributions to Mineralogy and Petrology
• 影响因子: 3.5
• 作者: Boulliung J

The bonding environment of chlorine in silicate melts

硅酸盐熔体中氯的结合环境

• DOI: 10.1016/j.chemgeo.2022.121269
• 发表时间: 2023
• 期刊: Chemical Geology
• 影响因子: 3.9
• 作者: Thomas R

Compositional and temperature effects on sulfur speciation and solubility in silicate melts

• DOI: 10.1016/j.epsl.2018.12.006
• 发表时间: 2019-02
• 期刊: Earth and Planetary Science Letters
• 影响因子: 5.3
• 作者: William M. Nash;D. Smythe;B. Wood

SO2 solubility and degassing behavior in silicate melts

• DOI: 10.1016/j.gca.2022.08.032
• 发表时间: 2022-09-19
• 期刊: GEOCHIMICA ET COSMOCHIMICA ACTA
• 影响因子: 5
• 作者: Boulliung, Julien;Wood, Bernard J.
• 通讯作者: Wood, Bernard J.