{"title":"太阳系研究中心近地小行星光曲线分析:2018年7月至9月。","authors":"Brian D Warner, Robert D Stephens","doi":"","DOIUrl":null,"url":null,"abstract":"<p><p>Lightcurves for 45 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 July-September were analyzed for rotation period and signs of satellites or tumbling. NEA 13553 Massakikoyama appears to be in non-principal axis rotation, i.e., tumbling. 2011 UA (<i>D</i> = 0.6 km) is a super-fast rotator with a period of 0.316391 ± 0.000007 h. The period and size place it well above the spin barrier. The period for 2018 RQ2 is multiply ambiguous, with possible solutions of 4.28 h or 5.17 h (monomdal lightcurve) and 8.58 h or 10.60 h (bimodal lightcurve). 2018 KE3 may be a binary asteroid.</p>","PeriodicalId":75145,"journal":{"name":"The Minor planet bulletin","volume":"46 1","pages":"27-40"},"PeriodicalIF":0.0000,"publicationDate":"2019-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7243871/pdf/nihms-1570169.pdf","citationCount":"0","resultStr":"{\"title\":\"NEAR-EARTH ASTEROID LIGHTCURVE ANALYSIS AT THE CENTER FOR SOLAR SYSTEM STUDIES: 2018 JULY-SEPTEMBER.\",\"authors\":\"Brian D Warner, Robert D Stephens\",\"doi\":\"\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<p><p>Lightcurves for 45 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 July-September were analyzed for rotation period and signs of satellites or tumbling. NEA 13553 Massakikoyama appears to be in non-principal axis rotation, i.e., tumbling. 2011 UA (<i>D</i> = 0.6 km) is a super-fast rotator with a period of 0.316391 ± 0.000007 h. The period and size place it well above the spin barrier. The period for 2018 RQ2 is multiply ambiguous, with possible solutions of 4.28 h or 5.17 h (monomdal lightcurve) and 8.58 h or 10.60 h (bimodal lightcurve). 2018 KE3 may be a binary asteroid.</p>\",\"PeriodicalId\":75145,\"journal\":{\"name\":\"The Minor planet bulletin\",\"volume\":\"46 1\",\"pages\":\"27-40\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2019-01-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7243871/pdf/nihms-1570169.pdf\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The Minor planet bulletin\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The Minor planet bulletin","FirstCategoryId":"1085","ListUrlMain":"","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
摘要
对2018年7月至9月在太阳系研究中心(CS3)获得的45颗近地小行星(NEAs)的光曲线进行了分析，以确定其旋转周期和卫星或翻转的迹象。NEA 13553 masakikoyama看起来是非主轴旋转，即翻滚。2011 UA (D = 0.6 km)是一个周期为0.316391±0.000007小时的超高速旋转体。周期和大小使其远远超过自旋势障。2018年RQ2的周期是多重模糊的，可能的解决方案为4.28小时或5.17小时(单峰光曲线)和8.58小时或10.60小时(双峰光曲线)。2018 KE3可能是一颗双星小行星。
NEAR-EARTH ASTEROID LIGHTCURVE ANALYSIS AT THE CENTER FOR SOLAR SYSTEM STUDIES: 2018 JULY-SEPTEMBER.
Lightcurves for 45 Near-Earth asteroids (NEAs) obtained at the Center for Solar System Studies (CS3) from 2018 July-September were analyzed for rotation period and signs of satellites or tumbling. NEA 13553 Massakikoyama appears to be in non-principal axis rotation, i.e., tumbling. 2011 UA (D = 0.6 km) is a super-fast rotator with a period of 0.316391 ± 0.000007 h. The period and size place it well above the spin barrier. The period for 2018 RQ2 is multiply ambiguous, with possible solutions of 4.28 h or 5.17 h (monomdal lightcurve) and 8.58 h or 10.60 h (bimodal lightcurve). 2018 KE3 may be a binary asteroid.
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号
