Estimation of Ejecta Thickness from Impact Craters in the South Polar Region of the Moon
— The paper presents the results of model calculations of impact craters ejecta thickness variations in the south polar region of the Moon from the south pole to 70° S for craters of Nectarian, Imbrian, Eratosthenian, and Copernican ages. This work does not consider pre-Nectarian craters since young...
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| Veröffentlicht in: | Solar system research 2023-04, Vol.57 (2), p.122-132 |
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| creator | Krasilnikov, A. S. Krasilnikov, S. S. Ivanov, M. A. Head, J. W. |
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The paper presents the results of model calculations of impact craters ejecta thickness variations in the south polar region of the Moon from the south pole to 70° S for craters of Nectarian, Imbrian, Eratosthenian, and Copernican ages. This work does not consider pre-Nectarian craters since younger deposits often hide the boundaries of their ejecta. Housen, Sharpton and Fassett models were chosen to estimate the power. The first was used for craters larger than 45 km in diameter, the second for smaller craters (from 3 to 45 km), and the third for the Mare Orientale basin. During estimation, the mixing factor of ejecta with the underlying regolith (factor μ) was considered. As a result, maps of ejecta thicknesses were produced for the Moon’s south polar region. They provide an opportunity for quantitative estimation of the various aged impact events’ contribution to the formation of polar regolith and, accordingly, to determine the dominant source (sources) of material in a particular area, not least in the proposed landing sites. |
| doi_str_mv | 10.1134/S0038094623020041 |
| format | Article |
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The paper presents the results of model calculations of impact craters ejecta thickness variations in the south polar region of the Moon from the south pole to 70° S for craters of Nectarian, Imbrian, Eratosthenian, and Copernican ages. This work does not consider pre-Nectarian craters since younger deposits often hide the boundaries of their ejecta. Housen, Sharpton and Fassett models were chosen to estimate the power. The first was used for craters larger than 45 km in diameter, the second for smaller craters (from 3 to 45 km), and the third for the Mare Orientale basin. During estimation, the mixing factor of ejecta with the underlying regolith (factor μ) was considered. As a result, maps of ejecta thicknesses were produced for the Moon’s south polar region. They provide an opportunity for quantitative estimation of the various aged impact events’ contribution to the formation of polar regolith and, accordingly, to determine the dominant source (sources) of material in a particular area, not least in the proposed landing sites.</description><identifier>ISSN: 0038-0946</identifier><identifier>EISSN: 1608-3423</identifier><identifier>DOI: 10.1134/S0038094623020041</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Astronomy ; Astrophysics and Astroparticles ; Astrophysics and Cosmology ; Observations and Techniques ; Physics ; Physics and Astronomy ; Planetology</subject><ispartof>Solar system research, 2023-04, Vol.57 (2), p.122-132</ispartof><rights>Pleiades Publishing, Inc. 2023. ISSN 0038-0946, Solar System Research, 2023, Vol. 57, No. 2, pp. 122–132. © Pleiades Publishing, Inc., 2023. Russian Text © The Author(s), 2023, published in Astronomicheskii Vestnik, 2023, Vol. 57, No. 2, pp. 124–135.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c218t-40d20f4886c15710d81d16aa8446aa940c25142b62e77a5e4852566fd55e29313</citedby><cites>FETCH-LOGICAL-c218t-40d20f4886c15710d81d16aa8446aa940c25142b62e77a5e4852566fd55e29313</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1134/S0038094623020041$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1134/S0038094623020041$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,780,784,27924,27925,41488,42557,51319</link.rule.ids></links><search><creatorcontrib>Krasilnikov, A. S.</creatorcontrib><creatorcontrib>Krasilnikov, S. S.</creatorcontrib><creatorcontrib>Ivanov, M. A.</creatorcontrib><creatorcontrib>Head, J. W.</creatorcontrib><title>Estimation of Ejecta Thickness from Impact Craters in the South Polar Region of the Moon</title><title>Solar system research</title><addtitle>Sol Syst Res</addtitle><description>—
The paper presents the results of model calculations of impact craters ejecta thickness variations in the south polar region of the Moon from the south pole to 70° S for craters of Nectarian, Imbrian, Eratosthenian, and Copernican ages. This work does not consider pre-Nectarian craters since younger deposits often hide the boundaries of their ejecta. Housen, Sharpton and Fassett models were chosen to estimate the power. The first was used for craters larger than 45 km in diameter, the second for smaller craters (from 3 to 45 km), and the third for the Mare Orientale basin. During estimation, the mixing factor of ejecta with the underlying regolith (factor μ) was considered. As a result, maps of ejecta thicknesses were produced for the Moon’s south polar region. They provide an opportunity for quantitative estimation of the various aged impact events’ contribution to the formation of polar regolith and, accordingly, to determine the dominant source (sources) of material in a particular area, not least in the proposed landing sites.</description><subject>Astronomy</subject><subject>Astrophysics and Astroparticles</subject><subject>Astrophysics and Cosmology</subject><subject>Observations and Techniques</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Planetology</subject><issn>0038-0946</issn><issn>1608-3423</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><recordid>eNp9kM1OwzAQhC0EEqXwANz8AoFd_8U9oqhApSIQLRK3yDhOk9LEle0eeHsStTckLruH2W-0M4TcItwhcnG_AuAaZkIxDgxA4BmZoAKdccH4OZmMcjbql-Qqxi0AAuRqQj7nMbWdSa3vqa_pfOtsMnTdtPa7dzHSOviOLrq9sYkWwSQXIm17mhpHV_6QGvrmdybQd7c5OYzKi_f9NbmozS66m9Oeko_H-bp4zpavT4viYZlZhjplAioGtdBaWZQ5QqWxQmWMFmKYMwGWSRTsSzGX50Y6oSWTStWVlI7NOPIpwaOvDT7G4OpyH4ZA4adEKMdqyj_VDAw7MnG47TculFt_CP3w5j_QL38VY6U</recordid><startdate>20230401</startdate><enddate>20230401</enddate><creator>Krasilnikov, A. S.</creator><creator>Krasilnikov, S. S.</creator><creator>Ivanov, M. A.</creator><creator>Head, J. W.</creator><general>Pleiades Publishing</general><scope>AAYXX</scope><scope>CITATION</scope></search><sort><creationdate>20230401</creationdate><title>Estimation of Ejecta Thickness from Impact Craters in the South Polar Region of the Moon</title><author>Krasilnikov, A. S. ; Krasilnikov, S. S. ; Ivanov, M. A. ; Head, J. W.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c218t-40d20f4886c15710d81d16aa8446aa940c25142b62e77a5e4852566fd55e29313</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Astronomy</topic><topic>Astrophysics and Astroparticles</topic><topic>Astrophysics and Cosmology</topic><topic>Observations and Techniques</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Planetology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Krasilnikov, A. S.</creatorcontrib><creatorcontrib>Krasilnikov, S. S.</creatorcontrib><creatorcontrib>Ivanov, M. A.</creatorcontrib><creatorcontrib>Head, J. W.</creatorcontrib><collection>CrossRef</collection><jtitle>Solar system research</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Krasilnikov, A. S.</au><au>Krasilnikov, S. S.</au><au>Ivanov, M. A.</au><au>Head, J. W.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Estimation of Ejecta Thickness from Impact Craters in the South Polar Region of the Moon</atitle><jtitle>Solar system research</jtitle><stitle>Sol Syst Res</stitle><date>2023-04-01</date><risdate>2023</risdate><volume>57</volume><issue>2</issue><spage>122</spage><epage>132</epage><pages>122-132</pages><issn>0038-0946</issn><eissn>1608-3423</eissn><abstract>—
The paper presents the results of model calculations of impact craters ejecta thickness variations in the south polar region of the Moon from the south pole to 70° S for craters of Nectarian, Imbrian, Eratosthenian, and Copernican ages. This work does not consider pre-Nectarian craters since younger deposits often hide the boundaries of their ejecta. Housen, Sharpton and Fassett models were chosen to estimate the power. The first was used for craters larger than 45 km in diameter, the second for smaller craters (from 3 to 45 km), and the third for the Mare Orientale basin. During estimation, the mixing factor of ejecta with the underlying regolith (factor μ) was considered. As a result, maps of ejecta thicknesses were produced for the Moon’s south polar region. They provide an opportunity for quantitative estimation of the various aged impact events’ contribution to the formation of polar regolith and, accordingly, to determine the dominant source (sources) of material in a particular area, not least in the proposed landing sites.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.1134/S0038094623020041</doi><tpages>11</tpages></addata></record> |
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| subjects | Astronomy Astrophysics and Astroparticles Astrophysics and Cosmology Observations and Techniques Physics Physics and Astronomy Planetology |
| title | Estimation of Ejecta Thickness from Impact Craters in the South Polar Region of the Moon |
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