流不稳定性在月球和外月形成过程中的有限作用

IF 3.8 Q2 ASTRONOMY & ASTROPHYSICS The Planetary Science Journal Pub Date : 2024-06-16 DOI:10.3847/psj/ad4863
Miki Nakajima, Jeremy Atkins, Jacob B. Simon and Alice C. Quillen
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引用次数: 0

摘要

人们普遍认为,月球是由原地球和撞击器之间的撞击所形成的圆盘吸积而成的,但其细节却存在很大争议。一些模型认为,火星大小的撞击器在地球周围形成了一个富含硅酸盐熔体(蒸汽贫乏)的圆盘,而另一些模型则认为,高能撞击产生了一个富含硅酸盐蒸汽的圆盘。然而,这种富含水汽的圆盘可能并不适合月球的形成,因为半径为 100 米至 100 千米的小卫星(月球的组成部分)可能会受到强大的气体阻力,在短时间内坠落到地球上,无法继续生长。如果大型小月体(≫100 千米)通过流不稳定性迅速形成,这个问题就可以避免。流不稳定性是一个将粒子集中到足以导致引力塌缩并迅速形成小行星或小月的过程。在这里,我们首次研究了成月盘中流不稳定性的影响,发现这种不稳定性可以快速形成∼100 公里大小的小月。然而,这些小月并没有大到足以避开强大阻力的程度,它们仍然会很快落到地球上。这表明富含蒸汽的磁盘可能不会形成大卫星,因此产生贫蒸汽磁盘的模型得到了支持。这一结果适用于一般的撞击诱发的卫星形成盘,支持了之前的建议,即小行星(<1.6 R⊕)是承载大卫星的良好候选者,因为它们的撞击诱发盘很可能是贫蒸汽的。我们发现流不稳定性在撞击诱发盘中卫星形成过程中的作用有限,而在行星形成过程中却起着关键作用。
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The Limited Role of the Streaming Instability during Moon and Exomoon Formation
It is generally accepted that the Moon accreted from the disk formed by an impact between the proto-Earth and impactor, but its details are highly debated. Some models suggest that a Mars-sized impactor formed a silicate melt-rich (vapor-poor) disk around Earth, whereas other models suggest that a highly energetic impact produced a silicate vapor-rich disk. Such a vapor-rich disk, however, may not be suitable for the Moon formation, because moonlets, building blocks of the Moon, of 100 m–100 km in radius may experience strong gas drag and fall onto Earth on a short timescale, failing to grow further. This problem may be avoided if large moonlets (≫100 km) form very quickly by streaming instability, which is a process to concentrate particles enough to cause gravitational collapse and rapid formation of planetesimals or moonlets. Here, we investigate the effect of the streaming instability in the Moon-forming disk for the first time and find that this instability can quickly form ∼100 km-sized moonlets. However, these moonlets are not large enough to avoid strong drag, and they still fall onto Earth quickly. This suggests that the vapor-rich disks may not form the large Moon, and therefore the models that produce vapor-poor disks are supported. This result is applicable to general impact-induced moon-forming disks, supporting the previous suggestion that small planets (<1.6 R⊕) are good candidates to host large moons because their impact-induced disks would likely be vapor-poor. We find a limited role of streaming instability in satellite formation in an impact-induced disk, whereas it plays a key role during planet formation.
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来源期刊
The Planetary Science Journal
The Planetary Science Journal Earth and Planetary Sciences-Geophysics
CiteScore
5.20
自引率
0.00%
发文量
249
审稿时长
15 weeks
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