标题： 原行星盘的形成和演化：结合观测、模拟和宇宙化学约束 显示英文标题

标题： Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints

摘要： 我们提出了一种对原太阳盘演化的合理且连贯的观点，该观点与宇宙化学约束一致，并与其它原行星盘的观测结果以及复杂的数值模拟相兼容。 高温度冷凝物、钙铝富含物（CAIs）和氧化铝球粒（AOAs）在原太阳附近形成，随后被输送到外盘的证据，可以通过盘早期剧烈的径向扩展阶段来解释，或者通过原恒星喷流将这些冷凝物快速从原太阳附近输送到大半径盘区来解释。 假设在吸积过程结束时吸积的物质具有同位素特征差异，使我们能够解释陨石中核合成同位素异常的观察到的二分法，并导致对彗星中难熔元素同位素组成的有趣预测。 当物质吸积减弱时，盘开始作为吸积盘演化。 最初，尘埃向内漂移，使尘埃组分的半径缩小至约45天文单位，可能约为气体组分宽度的一半。 然后必须出现了结构，在盘中产生一系列压力极大值，这些压力极大值在My时间尺度上捕获了尘埃。 这使得行星esimal在截然不同的时间形成，而其同位素特性没有显著变化。 没有通过流束向盘后期吸积物质。 根据陨石中的古磁数据，盘在约5 Myr内消失。 总之，原太阳盘的演化似乎在大小、寿命和尘埃行为方面相当典型，这表明太阳系相对于系外行星系统的特殊性可能源于行星形成的混沌性质，而不是来自母盘层面。 显示英文摘要

摘要： We present a plausible and coherent view of the evolution of the protosolar disk that is consistent with the cosmochemical constraints and compatible with observations of other protoplanetary disks and sophisticated numerical simulations. The evidence that high-temperature condensates, CAIs and AOAs, formed near the protosun before being transported to the outer disk can be explained by either an early phase of vigorous radial spreading of the disk, or fast transport of these condensates from the vicinity of the protosun towards large disk radii via the protostellar outflow. The assumption that the material accreted towards the end of the infall phase was isotopically distinct allows us to explain the observed dichotomy in nucleosynthetic isotopic anomalies of meteorites and leads to intriguing predictions on the isotopic composition of refractory elements in comets. When the infall of material waned, the disk started to evolve as an accretion disk. Initially, dust drifted inwards, shrinking the radius of the dust component to ~ 45 au, probably about 1/2 of the width of the gas component. Then structures must have emerged, producing a series of pressure maxima in the disk which trapped the dust on My timescales. This allowed planetesimals to form at radically distinct times without changing significantly of isotopic properties. There was no late accretion of material onto the disk via streamers. The disk disappeared in ~5 Myr, as indicated by paleomagnetic data in meteorites. In conclusion, the evolution of the protosolar disk seems to have been quite typical in terms of size, lifetime, and dust behavior, suggesting that the peculiarities of the Solar system with respect to extrasolar planetary system probably originate from the chaotic nature of planet formation and not at the level of the parental disk.