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arXiv 2301.02482astro-ph.EPastro-ph.SR
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原太阳星云中挥发物储层的演化

Evolution of the reservoirs of volatiles in the protosolar nebula

Antoine Schneeberger, Olivier Mousis, Artyom Aguichine, Jonathan I. Lunine

备注：
To be published in Astronomy & Astrophysics 19 pages, 11 figures
发表信息：
A&A 670, A28 (2023)
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摘要：

在巨行星中观察到的挥发物的超日丰度表明，在原太阳星云中形成时存在成分梯度。为了解释这种梯度，一些研究已经调查了微量物质的径向运输和冰对盘中形成的固体和蒸气的丰度分布的影响。然而，这些模型只考虑了在原太阳星云演化过程中存在的纯凝聚物或无定形冰形式的固体。他们通常忽略了可能的结晶和不稳定的笼形物，以及由此产生的相互作用之间的丰富的水和这些结晶形式。这项研究的目的是通过考虑原太阳星云中所有可能的固态相：纯凝聚物，无定形冰和笼形物来进一步推动这种研究。为此，我们使用了一个一维（1D）的原行星盘模型，再加上模块描述的气相中的痕量物种的演变，以及灰尘和鹅卵石的动力学。其中包括H $_2$ O，CO，CO $_2$，CH $_4$，H $_2$ S，N $_2$，NH $_3$，Ar，Kr，NH2，和PH $_3$等11个关键物种。两套初始条件的原太阳星云进行了探讨。在第一种情况下，圆盘最初充满了纯冷凝物形式的冰颗粒。在这种情况下，我们表明，包合物可以结晶，并形成富集峰高达约10倍的初始丰度在其结晶线。在第二种情况下，挥发物以无定形颗粒的形式被输送到原太阳星云。在这种情况下，笼形物的存在是不可能的，因为在它们的形成区域中没有可用的结晶水冰。纯凝析物的浓缩峰也在雪线之外形成，达到初始丰度的约7倍。

英文摘要：

The supersolar abundances of volatiles observed in giant planets suggest that a compositional gradient was present at the time of their formation in the protosolar nebula. To explain this gradient, several studies have investigated the radial transport of trace species and the effect of icelines on the abundance profiles of solids and vapors formed in the disk. However, these models only consider the presence of solids in the forms of pure condensates or amorphous ice during the evolution of the protosolar nebula. They usually neglect the possible crystallization and destabilization of clathrates, along with the resulting interplay between the abundance of water and those of these crystalline forms. This study is aimed at pushing this kind of investigation further by considering all possible solid phases together in the protosolar nebula: pure condensates, amorphous ice, and clathrates. To this end, we used a one-dimensional (1D) protoplanetary disk model coupled with modules describing the evolution of trace species in the vapor phase, as well as the dynamics of dust and pebbles. Eleven key species are considered here, including H$_2$O, CO, CO$_2$, CH$_4$, H$_2$S, N$_2$, NH$_3$, Ar, Kr, Xe, and PH$_3$. Two sets of initial conditions are explored for the protosolar nebula. In a first scenario, the disk is initially filled with icy grains in the forms of pure condensates. In this case, we show that clathrates can crystallize and form enrichment peaks up to about ten times the initial abundances at their crystallization lines. In a second scenario, the volatiles were delivered to the protosolar nebula in the forms of amorphous grains. In this case, the presence of clathrates is not possible because there is no available crystalline water ice in their formation region. Enrichment peaks of pure condensates also form beyond the snowline up to about seven times the initial abundances.

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