{"title":"近地小行星(6053)1993 bw3的光曲线分析。","authors":"Brian D Warner","doi":"","DOIUrl":null,"url":null,"abstract":"<p><p>CCD photometric observations of the near-Earth asteroid (6053) 1993 BW3 were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January and March. Analysis of the individual and combined data sets produced a period on the order of 2.8 hours. This differs significantly from the results of Pravec et al. (1997; <i>P</i> = 2.573 h) and from shape models by Durech (2002) and Kaasalainen (2002). While this discordance is not resolved, the 2.573 h value has the greatest amount of data supporting it, and for now, remains the favored period solution.</p>","PeriodicalId":75145,"journal":{"name":"The Minor planet bulletin","volume":"42 4","pages":"254-256"},"PeriodicalIF":0.0000,"publicationDate":"2015-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7244092/pdf/nihms-1570078.pdf","citationCount":"0","resultStr":"{\"title\":\"LIGHTCURVE ANALYSIS OF THE NEAR-EARTH ASTEROID (6053) 1993 BW3.\",\"authors\":\"Brian D Warner\",\"doi\":\"\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<p><p>CCD photometric observations of the near-Earth asteroid (6053) 1993 BW3 were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January and March. Analysis of the individual and combined data sets produced a period on the order of 2.8 hours. This differs significantly from the results of Pravec et al. (1997; <i>P</i> = 2.573 h) and from shape models by Durech (2002) and Kaasalainen (2002). While this discordance is not resolved, the 2.573 h value has the greatest amount of data supporting it, and for now, remains the favored period solution.</p>\",\"PeriodicalId\":75145,\"journal\":{\"name\":\"The Minor planet bulletin\",\"volume\":\"42 4\",\"pages\":\"254-256\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2015-10-01\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7244092/pdf/nihms-1570078.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}
LIGHTCURVE ANALYSIS OF THE NEAR-EARTH ASTEROID (6053) 1993 BW3.
CCD photometric observations of the near-Earth asteroid (6053) 1993 BW3 were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January and March. Analysis of the individual and combined data sets produced a period on the order of 2.8 hours. This differs significantly from the results of Pravec et al. (1997; P = 2.573 h) and from shape models by Durech (2002) and Kaasalainen (2002). While this discordance is not resolved, the 2.573 h value has the greatest amount of data supporting it, and for now, remains the favored period solution.
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