The Impact of Serpentinization on the Initial Conditions of Satellite Forming Collisions of Large Kuiper Belt Objects

IF 3.3 3区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Publications of the Astronomical Society of the Pacific Pub Date : 2023-12-08 DOI:10.1088/1538-3873/ad0f9a
A. Farkas-Takács, Csaba Kiss
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Abstract

Kuiper Belt objects are thought to be formed at least a few million years after the formation of calcium–aluminum-rich inclusions (CAIs), at a time when the 26Al isotope—the major source of radiogenic heat in the early solar system—had significantly depleted. The internal structure of these objects is highly dependent on any additional source that can produce extra heat in addition to that produced by the remaining, long-lasting radioactive isotopes. In this paper, we explore how serpentinization, the hydration of silicate minerals, can contribute to the heat budget and to what extent it can modify the internal structure of large Kuiper Belt objects. We find that the extent of restructuring depends very strongly on the start time of the formation process, the size of the object, and the starting ice-to-rock ratio. Serpentinization is able to restructure most of the interior of all objects in the whole size range (400–1200 km) and ice-to-rock ratio range investigated if the process starts early, ∼3 Myr after CAI formation, potentially leading to a predominantly serpentine core much earlier than previously thought (≤5 Myr versus several tens of million years). While the ratio of serpentinized material gradually decreases with the increasing formation time, the increasing ice-to-rock ratio, and the increasing start time of planetesimal formation in the outer solar system, in the case of the largest objects a significant part of the interior will be serpentinized even if the formation starts relatively late, ∼5 Myr after CAI formation. Therefore it is feasible that the interior of planetesimals may have contained a significant amount of serpentine, and in some cases, it could have been a dominant constituent, at the time of satellite-forming impacts.
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蛇形化对柯伊伯带大型天体卫星形成碰撞初始条件的影响
柯伊伯带天体被认为是在富钙铝包裹体(CAIs)形成至少几百万年后形成的,当时26Al同位素——早期太阳系中放射性热的主要来源——已经明显耗尽。这些物体的内部结构高度依赖于任何可以产生额外热量的额外来源,除了剩余的、持久的放射性同位素产生的热量。在本文中,我们探讨了蛇纹石化,硅酸盐矿物的水化作用,如何有助于热收支,以及它在多大程度上可以改变大型柯伊伯带天体的内部结构。我们发现,重构的程度在很大程度上取决于形成过程的开始时间、物体的大小和开始的冰岩比。蛇纹石化能够在整个尺寸范围(400-1200公里)内重构所有物体的大部分内部,如果这一过程开始得早,在CAI形成后约3 Myr,可能导致以蛇纹石为主的核心比以前认为的要早得多(≤5 Myr,而不是几千万年前)。蛇纹石化物质的比例随着形成时间的增加、冰岩比的增加和外太阳系星子形成开始时间的增加而逐渐减少,但对于最大的天体来说,即使形成开始得相对较晚,在CAI形成后约5 Myr,内部也有很大一部分会被蛇纹石化。因此,小星子的内部可能含有大量的蛇纹石,在某些情况下,在形成卫星的撞击中,蛇纹石可能是主要成分。
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来源期刊
Publications of the Astronomical Society of the Pacific
Publications of the Astronomical Society of the Pacific 地学天文-天文与天体物理
CiteScore
6.70
自引率
5.70%
发文量
103
审稿时长
4-8 weeks
期刊介绍: The Publications of the Astronomical Society of the Pacific (PASP), the technical journal of the Astronomical Society of the Pacific (ASP), has been published regularly since 1889, and is an integral part of the ASP''s mission to advance the science of astronomy and disseminate astronomical information. The journal provides an outlet for astronomical results of a scientific nature and serves to keep readers in touch with current astronomical research. It contains refereed research and instrumentation articles, invited and contributed reviews, tutorials, and dissertation summaries.
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