早期太阳系及其流星见证者

Emmanuel Jacquet, Cornelis Dullemond, Joanna Drążkowska, Steven Desch
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摘要

陨石,尤其是原始陨石(软玉),是太阳原行星盘不可替代的探测器。我们回顾了陨石的基本特性,并努力将它们置于天体物理学背景中。太阳系最早的固体,即难熔包裹体,可能形成于太阳系盘的最内层,并在其膨胀或扰动扩散的作用下向外迁移。如果软玉成分是在最大压力下被捕获的,那么它们的年龄分布可能与阻力引起的径向漂移趋势相一致,这可能是非碳质/碳质陨石同位素二分法的原因。如果将软玉解释为星云(非撞击)产物的话,那么软玉所具有的大约为一的固体/气体比率表明,在这些位置存在着有效的径向聚集和沉降,有利于通过流不稳定性形成行星。压力凸起的原因,如木星或凝结线,仍有待确定。
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The early Solar System and its meteoritical witnesses
Meteorites, and in particular primitive meteorites (chondrites), are irreplaceable probes of the solar protoplanetary disk. We review their essential properties and endeavour to place them in astrophysical context. The earliest solar system solids, refractory inclusions, may have formed over the innermost au of the disk and have been transported outward by its expansion or turbulent diffusion. The age spread of chondrite components may be reconciled with the tendency of drag-induced radial drift if they were captured in pressure maxima, which may account for the non-carbonaceous/carbonaceous meteorite isotopic dichotomy. The solid/gas ratio around unity witnessed by chondrules, if interpreted as nebular (non-impact) products, suggests efficient radial concentration and settling at such locations, conducive to planetesimal formation by the streaming instability. The cause of the pressure bumps, e.g. Jupiter or condensation lines, remains to be ascertained.
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