PengYue Wang , Edward Cloutis , Ye Su , PengFei Zhang
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引用次数: 0
Abstract
The establishment of robust meteorite-asteroid links has been a major focus of planetary exploration, and a major driver of asteroid sample return missions. Reflectance spectroscopy has been shown to be a powerful tool for this purpose. For the meteorites dominated by silicate minerals, quantitative analysis of spectral absorption features caused by the Fe2+-bearing minerals (mainly olivine and pyroxene) is a common method to determine mafic silicate mineralogy and end member abundances, and establish the relationship between them and possible parent bodies. In this study, the reflectance spectra of 22 primitive achondrites (acapulcoites, lodranites and winonaites) from NASA RELAB database were analyzed to determine their positions in the plot of the band area ratio (BAR) and 1 μm band center (Band I center). We found that Band I center and BAR of acapulcoites and lodranites are in roughly the same range. Acapulcoite-lodranite partially overlap with the field of H chondrites in the plot of the BAR and Band I center. This overlap means that spectral calibrations (also referred to as mineralogical formulas) based on the two types of meteorites needs to be applied with caution. The 2 μm band center of acapulcoite–lodranite is significantly lower than that of H chondrites, which is consistent with the conclusion of previous studies and provides a means to separate these two groups. In addition, the choice of spectral parameter analysis techniques may be a potential error source in similar studies. We provide generalized spectral fields of primitive achondrites in the plot of the BAR and Band I center derived from two widely used technologies.
建立强大的陨石-小行星联系一直是行星探索的重点,也是小行星采样返回任务的主要驱动力。反射光谱法已被证明是实现这一目的的有力工具。对于以硅酸盐矿物为主的陨石,定量分析含 Fe2+ 的矿物(主要是橄榄石和辉石)引起的光谱吸收特征,是确定岩浆硅酸盐矿物学和最终成员丰度,以及建立它们与可能的母体之间关系的常用方法。本研究分析了 NASA RELAB 数据库中 22 个原始隐晶岩(acapulcoites、lodranites 和 winonaites)的反射光谱,以确定它们在波段面积比(BAR)和 1 μm 波段中心(Band I 中心)图中的位置。我们发现,阿卡普尔科岩和珞珈岩的带I中心和带面积比大致处于同一范围。在 BAR 和波段 I 中心的曲线图中,金合欢岩-绿泥石与 H chondrites 领域部分重叠。这种重叠意味着需要谨慎应用基于这两类陨石的光谱校准(也称为矿物学公式)。阿卡普尔科岩-钠长石的 2 μm 波段中心明显低于 H 型软玉,这与先前研究的结论一致,并提供了将这两类陨石区分开来的方法。此外,光谱参数分析技术的选择可能是类似研究中的一个潜在误差源。我们在 BAR 和波段 I 中心的图中提供了原始硬粒岩的通用光谱场,这些光谱场是由两种广泛使用的技术得出的。
期刊介绍:
Icarus is devoted to the publication of original contributions in the field of Solar System studies. Manuscripts reporting the results of new research - observational, experimental, or theoretical - concerning the astronomy, geology, meteorology, physics, chemistry, biology, and other scientific aspects of our Solar System or extrasolar systems are welcome. The journal generally does not publish papers devoted exclusively to the Sun, the Earth, celestial mechanics, meteoritics, or astrophysics. Icarus does not publish papers that provide "improved" versions of Bode''s law, or other numerical relations, without a sound physical basis. Icarus does not publish meeting announcements or general notices. Reviews, historical papers, and manuscripts describing spacecraft instrumentation may be considered, but only with prior approval of the editor. An entire issue of the journal is occasionally devoted to a single subject, usually arising from a conference on the same topic. The language of publication is English. American or British usage is accepted, but not a mixture of these.