Dust from Supernovae in the Solar Nebula: An Integrated Nano- and Microanalytical Approach

太阳星云超新星尘埃：一种集成的纳米和微观分析方法

• 批准号: 248629227
• 负责人: Privatdozent Dr. Peter Hoppe
• 金额: --
• 依托单位: Max-Planck-Institut für Polymerforschung
• 依托单位国家: 德国
• 项目类别: Priority Programmes
• 财政年份: 2014
• 资助国家: 德国
• 起止时间: 2013-12-31 至 2016-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/248629227?language=en
• 关键词: Dust; Supernovae; Solar; Nebula; Integrated

Our Solar System formed from the collapse of an interstellar gas and dust cloud some 4.57 Gyr ago. Only a small fraction of the solid matter that went into the making of the Solar System survived the earliest stages of Solar System formation. Among this are so-called presolar grains, refractory, nanometer- to micrometer-sized high-temperature minerals, that are found in small quantities (up to several 100 ppm) in primitive Solar System materials. Presolar grains can be distinguished from solids that formed in the Solar System by their highly anomalous isotopic compositions. These relict grains formed in the winds of evolved stars or in the ejecta of nova and supernova (SN) explosions, i.e, they represent samples of stardust, captured by the forming planetary bodies in the early Solar System, that can be analyzed in great detail in the laboratory. Of particular importance are SiC and silicate dust grains from supernovae, the targets of this proposal. A comprehensive characterization of this Si-rich dust component, with detailed, simultaneous information on the isotopic compositions from light to heavy elements, and of the mineralogy will be important to better understand one of the building blocks from which our Solar System formed. Here, we aim to characterize this pristine dust component of the solar nebula in unrivaled detail at a scale of down to 50 nm (isotopes) and, respectively, of a few nm (mineralogy, subgrains). This will be achieved by the coordinated application of several nano- and microanalysis techniques to single SN dust grains.

我们的太阳系形成于大约4.57 Gyr前的星际气体和尘埃云的坍塌。只有一小部分进入太阳系形成的固体物质在太阳系形成的最早阶段幸存下来。其中包括所谓的前太阳颗粒，耐火，纳米到微米大小的高温矿物，在原始太阳系材料中发现少量（高达几百ppm）。前太阳颗粒可以通过其高度异常的同位素组成与太阳系中形成的固体区分开来。这些残留颗粒形成于演化恒星的风中或新星和超新星（SN）爆炸的喷出物中，也就是说，它们代表了星尘的样本，由早期太阳系形成的行星体捕获，可以在实验室中进行详细分析。特别重要的是来自超新星的SiC和硅酸盐尘埃颗粒，这是该提案的目标。这种富含Si的尘埃成分的全面表征，以及从轻到重元素的同位素组成和矿物学的详细信息，对于更好地了解我们太阳系形成的基石之一将是重要的。在这里，我们的目标是以无与伦比的细节来描述太阳星云的原始尘埃成分，其尺度分别为50 nm（同位素）和几nm（矿物学，亚晶粒）。这将通过对单个SN尘埃颗粒协调应用几种纳米和微量分析技术来实现。