Velbel Michael A, Zolensky Michael E
Department of Earth and Environmental Sciences Michigan State University 288 Farm Lane, Room 207, Natural Sciences Building East Lansing Michigan 48824-1115 USA.
Division of Meteorites Department of Mineral Sciences National Museum of Natural History Smithsonian Institution Washington District of Columbia 20013-7012 USA.
Meteorit Planet Sci. 2021 Mar;56(3):546-585. doi: 10.1111/maps.13636. Epub 2021 Apr 8.
The target bodies of C-complex asteroid sample return missions are carbonaceous chondrite-like near-Earth asteroids (NEAs), chosen for the abundance and scientific importance of their organic compounds and "hydrous" (including hydroxylated) minerals, such as serpentine-group phyllosilicates. Science objectives include returning samples of pristine carbonaceous regolith from asteroids for study of the nature, history, and distribution of its constituent minerals, organic material, and other volatiles. Heating after the natural aqueous alteration that formed the abundant phyllosilicates in CM and similar carbonaceous chondrites dehydroxylated them and altered or decomposed other volumetrically minor constituents (e.g., carbonates, sulfides, organic molecules; Tonui et al. 2003, 2014). We propose a peak-temperature thermometer based on dehydroxylation as measured by analytical totals from electron probe microanalysis (EPMA) of matrices in a number of heated and aqueously altered (but not further heated) CM chondrites. Some CM lithologies in Maribo and Sutter's Mill do not exhibit the matrix dehydroxylation expected for surface temperatures expected from insolation of meteoroids with their known orbital perihelia. This suggests that insolated-heated meteoroid surfaces were lost by ablation during passage through Earth's atmosphere, and that insolation-heated material is more likely to be encountered among returned asteroid regolith samples than in meteorites. More generally, several published lines of evidence suggest that episodic heating of some CM material, most likely by impacts, continued intermittently and locally up to billions of years after assembly and early heating of ancestral CM chondrite bodies. Mission spectroscopic measures of hydration can be used to estimate the extent of dehydroxylation, and the new dehydroxylation thermometer can be used directly to select fragments of returned samples most likely to contain less thermally altered inventories of primitive organic molecules.
C类小行星样本返回任务的目标天体是类碳质球粒陨石近地小行星(NEAs),之所以选择它们,是因为其有机化合物和“含水”(包括羟基化)矿物(如蛇纹石族层状硅酸盐)的丰富性和科学重要性。科学目标包括从小行星返回原始碳质风化层样本,以研究其组成矿物、有机物质和其他挥发物的性质、历史和分布。在CM及类似碳质球粒陨石中形成大量层状硅酸盐的自然水蚀变之后进行加热,会使它们脱羟基,并改变或分解其他体积较小的成分(如碳酸盐、硫化物、有机分子;托努伊等人,2003年、2014年)。我们提出一种基于脱羟基作用的峰值温度温度计,该脱羟基作用通过对一些加热过且经历了水蚀变(但未进一步加热)的CM球粒陨石基质进行电子探针微分析(EPMA)的分析总量来测量。马里博和萨特磨坊的一些CM岩性并未表现出根据具有已知轨道近日点的流星体日射所预期的表面温度下的基质脱羟基现象。这表明,在穿过地球大气层的过程中,经日射加热的流星体表面因烧蚀而损失,并且在返回的小行星风化层样本中比在陨石中更有可能遇到经日射加热的物质。更普遍地说,几条已发表的证据表明,一些CM物质的间歇性加热,最有可能是由撞击引起的,在原始CM球粒陨石母体聚集和早期加热之后数十亿年间持续间歇性地局部发生。任务中的水化光谱测量可用于估计脱羟基程度,而新的脱羟基温度计可直接用于选择返回样本中最有可能含有热改变程度较低的原始有机分子存量的碎片。