{"title":"THREE UNUSUAL HUNGARIA ASTEROIDS.","authors":"Brian D Warner","doi":"","DOIUrl":null,"url":null,"abstract":"<p><p>Three Hungaria asteroids observed at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January-March showed unusual characteristics. 2449 Kenos, a probable member of the Hungaria <i>collisional family,</i> is likely to be a binary object with period <i>P</i> <sub><i>1</i></sub> = 3.8481 h and <i>P</i> <sub><i>2</i></sub> = 15.85 h. The 2015 observations of 6901 Roybishop, a member of the Hungaria <i>orbital group</i>, showed signs of a weak secondary period, <i>P</i> <sub><i>2</i></sub> = 10.58 h. The secondary period is in contradiction with previous results. (23615) 1996 FK12 may be another example of so-called <i>wide binaries</i>, showing a strong short period, <i>P</i> <sub><i>2</i></sub> = 3.6456 h, presumably due to a widely-separated satellite that is not tidally locked to a very long orbital period. The primary in such a system has a very long period, <i>P</i> <sub><i>1</i></sub> = 368 h in this instance. The main question for 1996 FK12 is the validity of the long period.</p>","PeriodicalId":75145,"journal":{"name":"The Minor planet bulletin","volume":"42 3","pages":"183-186"},"PeriodicalIF":0.0000,"publicationDate":"2015-07-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7244151/pdf/nihms-1570072.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}
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Abstract
Three Hungaria asteroids observed at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) in 2015 January-March showed unusual characteristics. 2449 Kenos, a probable member of the Hungaria collisional family, is likely to be a binary object with period P1 = 3.8481 h and P2 = 15.85 h. The 2015 observations of 6901 Roybishop, a member of the Hungaria orbital group, showed signs of a weak secondary period, P2 = 10.58 h. The secondary period is in contradiction with previous results. (23615) 1996 FK12 may be another example of so-called wide binaries, showing a strong short period, P2 = 3.6456 h, presumably due to a widely-separated satellite that is not tidally locked to a very long orbital period. The primary in such a system has a very long period, P1 = 368 h in this instance. The main question for 1996 FK12 is the validity of the long period.
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