1 I/'Oumuamua可能是一个冰的分形集合体吗？
Could 1I/'Oumuamua be an icy fractal aggregate?
摘要：
1 I/'Oumuamua是第一个被探测到的星际闯入者，它显示了一种非重力加速度，这种加速度不能用释气来解释，因为从{ \it Spitzer}观测中可以明显看出释气的严格上限，除非普通挥发物的相对丰度与彗星中的挥发物非常不同。作为一种替代方案，有人建议，它的特殊加速度是由于辐射压力，需要一个未知的自然或人工起源的平面片几何形状。在这里，我们评估是否1 I/'Oumuamua的内部结构，而不是它的几何形状，可以支持辐射压力驱动的场景。我们采用了大量的分形结构，并发现，可以产生所需的面积与质量比的骨料的类型必须是非常多孔的，密度$\sim$ 10 $^{-5}$ g cm $^{-3}$。这样的多孔聚集体可以自然地产生于原行星盘雪线之外的冰尘颗粒的碰撞生长，我们认为1 I/'Oumuamua可能是这个种群的成员。这是一个值得研究的假设，因为如果是这样的话，1 I/'Oumuamua将打开一个新的观察窗口，研究其他恒星周围行星的组成部分。这可能会给行星形成模型带来前所未有的限制。\end{abstract}
英文摘要：
1I/'Oumuamua is the first interstellar interloper to be detected, and it shows a non-gravitational acceleration that cannot be accounted for by outgassing, given the strict upper limits of outgassing evident from {\it Spitzer} observations, unless the relative abundances of the common volatiles are very different to those in comets. As an alternative, it has been suggested that its peculiar acceleration is due to radiation pressure, requiring a planar-sheet geometry of an unknown natural or artificial origin. Here we assess whether or not the internal structure of 1I/'Oumuamua, rather than its geometry, could support a radiation-pressure-driven scenario. We adopt a mass fractal structure and find that the type of aggregate that could yield the required area-to-mass ratio would have to be extraordinarily porous, with a density $\sim$ 10$^{-5}$ g cm$^{-3}$. Such porous aggregates can naturally arise from the collisional grow of icy dust particles beyond the snowline of a protoplanetary disk, and we propose that 1I/'Oumuamua might be a member of this population. This is a hypothesis worth investigating because, if this were the case, 1I/'Oumuamua would have opened a new observation window on to the study of the building blocks of planets around other stars. This could set unprecedented constraints on planet formation models.\end{abstract}
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