Meteorite provenance and the asteroid connection
Meteorite provenance and the asteroid connection
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陨石起源与小行星的联系
DOI：
10.1144/gsl.sp.2006.256.01.19
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
A. J. Bowden
中科院分区：
文献类型：
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作者：
A. J. Bowden
摘要在我们的收藏中，陨石类型与小行星类别甚至单个小行星的匹配，也许可以说是从奥姆斯特德的陨石研究和1885年拍摄的Wienek开创性的流星摄影图像开始的。1960年代开始进行火球摄影网络调查，在此期间发起了三个主要的国家方案;每个方案都回收了一颗陨石，即Pamibram、迷城和Innisfree。虽然摄影测量的陨石回收率很低，但它们提供了关于近地空间流星体数量的宝贵数据。在将陨石与彗星或小行星的供应源联系起来时，动力学考虑是至关重要的。Ernst Öpik最初提出了一个问题，即确定在与已知陨石福尔斯坠落相匹配的时间尺度和流量内将小行星碎片运送到地球的机制。几名工作人员接受了奥皮克1963年的挑战，因此今天对小行星带内柯克伍德间隙的动力学条件和潜在的传递机制有了更好的了解。Brobovnikoff在1929年的开创性工作开创了小行星表面分光光度研究领域。他试图将小行星光谱与陨石的反射特性联系起来。仪器的进步导致麦考德在1969年开始了小行星分光光度研究的现代时代。这是当代研究的一个新兴领域，在确定可能的陨石-小行星类联系，甚至可能的陨石-小行星匹配方面取得了一些成功，即灶神星陨石和霍瓦蒂-钙铝榴石-闪长岩（HED）陨石。然而，小行星表面的空间风化可能掩盖了小行星的真实反射特性。近年来，航天器飞越任务揭示了更多关于小行星表面形态的信息：特别是S级小行星（951）Gaspra，（243）Ida和C级小行星（253）Mathilde。小行星不再是光点或光谱曲线，而是具有不同表面形态和地质历史的天体。NEAR-舒梅克航天器在进行了为期一年的轨道使命之后于2001年在爱神星（433）上软着陆就是一个例子。然而，仍然很难将我们收藏的陨石与已知的小行星分类分布相协调，它们可能是不相容的集合。
Abstract The matching of meteorite types held in our collections to asteroid classes, and even individual asteroids, may perhaps be said to commence with Olmsted’s meteor researches and Wienek’s pioneering photographic meteor image taken in 1885. Photographic fireball network surveys started up during the 1960s and three major national programmes were initiated during this period; each resulting in the recovery of one meteorite, Přibram, Lost City and Innisfree. Although photographic surveys had low meteorite recovery rates they, nevertheless, provided invaluable data on the population of meteoroids in near-Earth space. Dynamical considerations are paramount in connecting meteorites with cometary or asteroidal sources of supply. Ernst Öpik originally raised the question of locating the mechanism for delivering asteroid fragments to Earth within a timescale and flux that matches known meteorite falls. Several workers took up Öpik’s 1963 challenge, so that today the dynamical conditions and potential delivery mechanisms existing at the Kirkwood Gaps within the asteroid belt are better understood. Pioneering work by Brobovnikoff in 1929 initiated the field of spectrophotometric studies of asteroid surfaces. He attempted to correlate asteroid spectra with the reflective properties of meteorites. Advances in instrumentation led McCord in 1969 to initiate the modern era of asteroid spectrophotometric studies. This is a burgeoning field of contemporary research that has had some success in identifying possible meteorite-asteroid class linkages and even possible meteorite-asteroid matches, i.e. Vesta and howardite-eucrite-diogenite (HED) meteorites. However, space weathering of asteroid surfaces may mask the true asteroidal reflectance characteristics. In recent years spacecraft flyby missions have revealed more about the surface morphologies of asteroids: notably the S class asteroids (951) Gaspra, (243) Ida and the C class asteroid (253) Mathilde. Asteroids are no longer points of light or spectral curves but are bodies with distinct surface morphologies and geological histories. This was exemplified by the soft landing of the NEAR-Shoemaker spacecraft on (433) Eros in 2001 after a year-long orbital mission. However, it is still difficult to reconcile the meteorites held in our collections with the known distribution of asteroid classes and it may be that they are possibly incompatible sets.