Experimental investigation of the formation of accretionary rims around chondrules and the formation of chondrite parent bodies

球粒陨石是最常见的一类陨石，主要由两种成分组成，球粒是毫米级的固体珠粒，而基质则由微米级的尘埃颗粒组成。这些辉长岩已被矿物学，化学和同位素非常好的分析，使其属性的详细信息是可用的。然而，球粒陨石母体在年轻太阳系中形成的物理条件大多是未知的。陨石的年龄测定表明，它们的形成可以追溯到我们太阳系的最初几百万年。自那时以来，球粒陨石母体基本保持不变，因此保留了其原始结构。因此，有关导致观察到的内部结构的物理过程的知识可以提供有价值的见解，在星子的形成时间，例如其典型的碰撞速度的主导过程。在这里，我们建议在实验室实验中研究前陨石物质的碰撞物理，并将实验结果与真实的陨石进行比较。除此之外，我们还将研究细粒球粒边缘的形成，这种边缘经常在许多陨石中发现，其起源仍然是一个有争议的问题。我们的研究结果将有助于确定年轻太阳系中较大天体形成的过程。

Chondrites are the most common class of meteorites, which mainly consist of two components, the chondrules, which are millimeter-sized solid beads, and the matrix, which consists of micrometer-sized dust grains. These chondrites have been mineralogically, chemically and isotopically very well analyzed so that detailed information of their properties is available. However, the physical conditions under which the chondrite parent bodies were formed in the young Solar System are mostly unknown. Age determination of the chondrites showed that their formation dates back to the very first few million years of our Solar System. Since then, the chondrite parent bodies have remained mostly unchanged and have, thus, preserved their pristine structures. Therefore, knowledge about the physical processes that lead to the observed internal structures can provide valuable insights into the dominant processes during the formation time of planetesimals, e.g. their typical collision velocities. Here we propose to investigate the collision physics of pre-chondritic materials in laboratory experiments and to compare the experimental outcomes with real chondritic meteorites. In addition to that, we will investigate the formation of fine-grained chondrule rims, which are frequently found in many chondrites and whose origin is still a matter of debate. The results of our investigations will help to identify the processes by which larger bodies form in the young Solar System.