{"title":"Estimation of the Rate of Slope Processes and Morphological Variability of Kilometer-Sized Impact Craters on the Moon","authors":"X. Kochubey, M. A. Ivanov","doi":"10.1134/s0038094624010052","DOIUrl":null,"url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>In order to estimate the rate of slope processes on the Moon, we studied the morphology and topographic configuration of 24 craters in the diameter range of 5–15 km. These craters are located in Mare Serenitatis, Mare Crisium, and Mare Fecunditatis, as well as in the continental terrain of Montes Apenninus. The craters were formed in three types of targets: (1) two-layered (continent, overlaid by a mare), (2) single-layered mare, and (3) single-layered continent. The topographic configuration was established for each crater, and the frequency–size distribution of overlapping craters on the walls and in the continuous ejecta zone was determined. The age of the craters was estimated (from 0.31 to 3.83 Gyr) based on the crater density in the ejecta zone. Comparing this density with the density on the walls allowed us to estimate the rate of slope processes. The rate of slope processes (<i>E</i>, mm/Myr) on the Moon is nonlinear and described by a power-law function <i>Е</i> = 4.39<i>А</i><sup>–1.03</sup>, where <i>А</i> is the age (Gyr). The estimated rates of slope processes in our study range from ~17 mm/Myr for the youngest crater to ~0.8 mm/Myr for the oldest crater. The studied craters represent stable landforms, and their configuration remains almost unchanged over billions of years. The target type has no significant influence on either the rate of slope processes or the changes in crater shape over time.</p>","PeriodicalId":778,"journal":{"name":"Solar System Research","volume":null,"pages":null},"PeriodicalIF":0.6000,"publicationDate":"2024-05-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Solar System Research","FirstCategoryId":"101","ListUrlMain":"https://doi.org/10.1134/s0038094624010052","RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q4","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
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Abstract
In order to estimate the rate of slope processes on the Moon, we studied the morphology and topographic configuration of 24 craters in the diameter range of 5–15 km. These craters are located in Mare Serenitatis, Mare Crisium, and Mare Fecunditatis, as well as in the continental terrain of Montes Apenninus. The craters were formed in three types of targets: (1) two-layered (continent, overlaid by a mare), (2) single-layered mare, and (3) single-layered continent. The topographic configuration was established for each crater, and the frequency–size distribution of overlapping craters on the walls and in the continuous ejecta zone was determined. The age of the craters was estimated (from 0.31 to 3.83 Gyr) based on the crater density in the ejecta zone. Comparing this density with the density on the walls allowed us to estimate the rate of slope processes. The rate of slope processes (E, mm/Myr) on the Moon is nonlinear and described by a power-law function Е = 4.39А–1.03, where А is the age (Gyr). The estimated rates of slope processes in our study range from ~17 mm/Myr for the youngest crater to ~0.8 mm/Myr for the oldest crater. The studied craters represent stable landforms, and their configuration remains almost unchanged over billions of years. The target type has no significant influence on either the rate of slope processes or the changes in crater shape over time.
期刊介绍：
Solar System Research publishes articles concerning the bodies of the Solar System, i.e., planets and their satellites, asteroids, comets, meteoric substances, and cosmic dust. The articles consider physics, dynamics and composition of these bodies, and techniques of their exploration. The journal addresses the problems of comparative planetology, physics of the planetary atmospheres and interiors, cosmochemistry, as well as planetary plasma environment and heliosphere, specifically those related to solar-planetary interactions. Attention is paid to studies of exoplanets and complex problems of the origin and evolution of planetary systems including the solar system, based on the results of astronomical observations, laboratory studies of meteorites, relevant theoretical approaches and mathematical modeling. Alongside with the original results of experimental and theoretical studies, the journal publishes scientific reviews in the field of planetary exploration, and notes on observational results.
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