原行星盘的形成与演化:观测、模拟与宇宙化学约束的结合

Alessandro Morbidelli, Yves Marrocchi, Adnan Ali Ahmad, Asmita Bhandare, Sebastien Charnoz, Benoit Commercon, Cornellis P. Dullemond, Tristan Guillot, Patrick Hennebelle, Yueh-Ning Lee, Francesco Lovascio, Raphael Marschall, Bernard Marty, Anaelle Maury, Okamoto Tamami
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引用次数: 0

摘要

我们对原质星盘的演化提出了一个合理而连贯的观点,它与宇宙化学约束相一致,并与对其他原质星盘的观测和复杂的数值模拟相匹配。有证据表明,高温冷凝物、CAIs和AOAs在被传送到外盘之前在原太阳附近形成,这可以用盘早期剧烈的径向扩张阶段,或者这些冷凝物通过原恒星外流从原太阳附近向大盘半径快速传送来解释。假定在内溢阶段末期喷出的物质在同位素上是不同的,我们就可以解释所观测到的陨石核合成同位素异常的两极分化现象,并对彗星中难熔元素的同位素组成做出引人入胜的预测。当物质流入减弱时,圆盘开始演变为吸积盘。最初,尘埃向内漂移,使尘埃部分的半径缩小到大约 45 au,大概是气体部分宽度的 1/2。然后,一定出现了一些结构,在圆盘中产生了一系列压力最大值,这些压力最大值在我的时间尺度上捕获了尘埃。这使得行星形成的时间截然不同,而同位素性质却没有发生显著变化。没有物质通过流线向圆盘的后期增殖。陨石中的古地磁数据表明,星盘在大约5 Myr后消失。总之,原太阳系盘的演化在大小、寿命和尘埃行为方面似乎都很典型,这表明太阳系相对于太阳系外行星系统的特殊性可能源于行星形成的混乱性质,而不是母盘的水平。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Formation and evolution of a protoplanetary disk: combining observations, simulations and cosmochemical constraints
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.
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