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EARLY AQUEOUS ACTIVITY ON PRIMITIVE METEORITE PARENT BODIES

机译：初级陨石母体的早期活动

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THE interstellar material from which the Solar System formed has been modified by many processes(1): evaporation and condensation in the solar nebula, accretion into protoplanetary bodies and post-accretion processes within these bodies, Meteorites provide a record of these events and their chronology(2), Carbonaceous CI chondrites are among the most primitive, undifferentiated meteorites(3-6), but nevertheless show evidence of post-accretion alteration(7); they contain carbonates that are believed to have formed by reactions between anhydrous CI precursor materials and circulating fluids in the meteorite parent body (or bodies), yet little is known about the nature of these reactions or the timescale on which they occurred, Here we report measurements of excess Cr-53-formed by the decay of short-lived Mn-53-in five carbonate fragments from the CI chondrites Orgueil and Ivuna. Our results show that aqueous alteration on small protoplanetary bodies must have begun less than 20 Myr after the time of formation of the oldest known solar-nebula condensates(2) (Allende refractory inclusions). This upper limit is much shorter than that of 50 Myr inferred from previous studies(8), and clearly establishes aqueous alteration as one of the earliest processes in the chemical evolution of the Solar System. [References: 21]
机译：形成太阳系的星际物质已通过许多过程进行了修改（1）：太阳星云中的蒸发和凝结，向原行星体的吸积和这些星体内的增生过程，陨石提供了这些事件及其历程的记录（2），碳质CI球粒陨石是最原始，未分化的陨石（3-6），但仍显示出增生后改变的证据（7）；它们含有碳酸盐，据认为是由无水CI前驱物材料与陨石母体中循环流体之间的反应形成的，但对于这些反应的性质或发生的时间尺度知之甚少，在这里我们报告CI球粒陨石Orgueil和Ivuna的五个碳酸盐碎片中由短命Mn-53的衰变形成的过量Cr-53的测量结果。我们的结果表明，在形成最古老的已知太阳星云凝结物（2）（阿连德耐火夹杂物）之后，小型原行星体上的水蚀变化必须开始于20 Myr以下。这个上限比以前研究得出的50 Myr上限要短得多（8），并且清楚地确定了水蚀是太阳系化学演化的最早过程之一。 [参考：21]

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