神戸大学附属図書館デジタルアーカイブ
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https://hdl.handle.net/20.500.14094/90004010
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2024-04-29
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90004010 (fulltext)
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2.01 MB
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ファイル出力
メタデータID
90004010
アクセス権
open access
出版タイプ
Accepted Manuscript
タイトル
Spatial distribution of impact craters on Deimos
著者
著者ID
A2026
研究者ID
1000000791550
KUID
https://kuid-rm-web.ofc.kobe-u.ac.jp/search/detail?systemId=c16797b574e7b49f520e17560c007669
著者名
Hirata, Naoyuki
平田, 直之
ヒラタ, ナオユキ
所属機関名
理学研究科
収録物名
Icarus
巻(号)
288
ページ
69-77
出版者
Elsevier
刊行日
2017-05-15
公開日
2019-06-01
抄録
Deimos, one of the Martian moons, has numerous impact craters. However, it is unclear whether crater saturation has been reached on this satellite. To address this issue, we apply a statistical test known as nearest-neighbor analysis to analyze the crater distribution of Deimos. When a planetary surface such as the Moon is saturated with impact craters, the spatial distribution of craters is generally changed from random to more ordered. We measured impact craters on Deimos from Viking and HiRISE images and found (1) that the power law of the size-frequency distribution of the craters is approximately −1.7, which is significantly shallower than those of potential impactors, and (2) that the spatial distribution of craters over 30 m in diameter cannot be statistically distinguished from completely random distribution, which indicates that the surface of Deimos is inconsistent with a surface saturated with impact craters. Although a crater size-frequency distribution curve with a slope of −2 is generally interpreted as indicating saturation equilibrium, it is here proposed that two competing mechanisms, seismic shaking and ejecta emplacement, have played a major role in erasing craters on Deimos and are therefore responsible for the shallow slope of this curve. The observed crater density may have reached steady state owing to the obliterations induced by the two competing mechanisms. Such an occurrence indicates that the surface is saturated with impact craters despite the random distribution of craters on Deimos. Therefore, this work proposes that the age determined by the current craters on Deimos reflects neither the age of Deimos itself nor that of the formation of the large concavity centered at its south pole because craters should be removed by later impacts. However, a few of the largest craters on Deimos may be indicative of the age of the south pole event.
キーワード
Mars
Satellites
Impact processes
Geological processes
Cratering
Phobos and Deimos
カテゴリ
理学研究科
学術雑誌論文
権利
©2017 Elsevier.
This manuscript version is made available under the CC-BY-NC-ND 4.0 license http://creativecommons.org/licenses/by-nc-nd/4.0/
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資源タイプ
journal article
言語
English (英語)
ISSN
0019-1035
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eISSN
1090-2643
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関連情報
DOI
https://doi.org/10.1016/j.icarus.2017.01.035
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