{"title":"2016年HO3的共轨道跃迁","authors":"Yi Qi, Dong Qiao","doi":"10.1007/s42064-021-0122-0","DOIUrl":null,"url":null,"abstract":"<div><p>In this paper, we investigate the orbital behavior of the transition between the quasisatellite (QS) and horseshoe (HS) motions of 2016 HO<sub>3</sub>. Based on the phase space structure in the Sun–Earth circular restricted three-body problem, we find that the surface of 2016 HO<sub>3</sub> in the torus space is a compound surface formed by QS and HS portions. Its co-orbital motion is therefore a QS–HS transition. 2016 HO<sub>3</sub> is currently located in a QS state, and its locus clings to the QS portion in the isosurface in agreement with the semi-analytical results. We provide a criterion to separate the QS and HS stages in the transition and obtain accurate incoming and outgoing epochs of the QS motion. We then propose an approximate curve to describe the locus of 2016 HO<sub>3</sub> in the <i>ω − e</i> projection. Virtual asteroids (VAs) near 2016 HO<sub>3</sub> in the isosurface were created to study the influence of the initial state of the QS–HS transition. We find that the duration of the QS state is mainly influenced by the loci in the <i>ω − e</i> projection. The VAs with large QS durations usually have longer loci across the QS region than those with shorter durations. In addition, although some VAs are close to 2016 HO<sub>3</sub> in the <i>ω</i> − <i>e</i> projection, their co-orbital behaviors are significantly different from that of the latter. This indicates that the QS–HS transition of 2016 HO<sub>3</sub> is sensitive to the (<i>ω</i>, <i>e</i>) position.</p><div><figure><div><div><picture><source><img></source></picture></div></div></figure></div></div>","PeriodicalId":52291,"journal":{"name":"Astrodynamics","volume":"7 1","pages":"3 - 14"},"PeriodicalIF":2.7000,"publicationDate":"2022-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s42064-021-0122-0.pdf","citationCount":"1","resultStr":"{\"title\":\"Co-orbital transition of 2016 HO3\",\"authors\":\"Yi Qi, Dong Qiao\",\"doi\":\"10.1007/s42064-021-0122-0\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<div><p>In this paper, we investigate the orbital behavior of the transition between the quasisatellite (QS) and horseshoe (HS) motions of 2016 HO<sub>3</sub>. Based on the phase space structure in the Sun–Earth circular restricted three-body problem, we find that the surface of 2016 HO<sub>3</sub> in the torus space is a compound surface formed by QS and HS portions. Its co-orbital motion is therefore a QS–HS transition. 2016 HO<sub>3</sub> is currently located in a QS state, and its locus clings to the QS portion in the isosurface in agreement with the semi-analytical results. We provide a criterion to separate the QS and HS stages in the transition and obtain accurate incoming and outgoing epochs of the QS motion. We then propose an approximate curve to describe the locus of 2016 HO<sub>3</sub> in the <i>ω − e</i> projection. Virtual asteroids (VAs) near 2016 HO<sub>3</sub> in the isosurface were created to study the influence of the initial state of the QS–HS transition. We find that the duration of the QS state is mainly influenced by the loci in the <i>ω − e</i> projection. The VAs with large QS durations usually have longer loci across the QS region than those with shorter durations. In addition, although some VAs are close to 2016 HO<sub>3</sub> in the <i>ω</i> − <i>e</i> projection, their co-orbital behaviors are significantly different from that of the latter. This indicates that the QS–HS transition of 2016 HO<sub>3</sub> is sensitive to the (<i>ω</i>, <i>e</i>) position.</p><div><figure><div><div><picture><source><img></source></picture></div></div></figure></div></div>\",\"PeriodicalId\":52291,\"journal\":{\"name\":\"Astrodynamics\",\"volume\":\"7 1\",\"pages\":\"3 - 14\"},\"PeriodicalIF\":2.7000,\"publicationDate\":\"2022-03-08\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"https://link.springer.com/content/pdf/10.1007/s42064-021-0122-0.pdf\",\"citationCount\":\"1\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Astrodynamics\",\"FirstCategoryId\":\"1087\",\"ListUrlMain\":\"https://link.springer.com/article/10.1007/s42064-021-0122-0\",\"RegionNum\":1,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q2\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astrodynamics","FirstCategoryId":"1087","ListUrlMain":"https://link.springer.com/article/10.1007/s42064-021-0122-0","RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q2","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
In this paper, we investigate the orbital behavior of the transition between the quasisatellite (QS) and horseshoe (HS) motions of 2016 HO3. Based on the phase space structure in the Sun–Earth circular restricted three-body problem, we find that the surface of 2016 HO3 in the torus space is a compound surface formed by QS and HS portions. Its co-orbital motion is therefore a QS–HS transition. 2016 HO3 is currently located in a QS state, and its locus clings to the QS portion in the isosurface in agreement with the semi-analytical results. We provide a criterion to separate the QS and HS stages in the transition and obtain accurate incoming and outgoing epochs of the QS motion. We then propose an approximate curve to describe the locus of 2016 HO3 in the ω − e projection. Virtual asteroids (VAs) near 2016 HO3 in the isosurface were created to study the influence of the initial state of the QS–HS transition. We find that the duration of the QS state is mainly influenced by the loci in the ω − e projection. The VAs with large QS durations usually have longer loci across the QS region than those with shorter durations. In addition, although some VAs are close to 2016 HO3 in the ω − e projection, their co-orbital behaviors are significantly different from that of the latter. This indicates that the QS–HS transition of 2016 HO3 is sensitive to the (ω, e) position.
期刊介绍：
Astrodynamics is a peer-reviewed international journal that is co-published by Tsinghua University Press and Springer. The high-quality peer-reviewed articles of original research, comprehensive review, mission accomplishments, and technical comments in all fields of astrodynamics will be given priorities for publication. In addition, related research in astronomy and astrophysics that takes advantages of the analytical and computational methods of astrodynamics is also welcome. Astrodynamics would like to invite all of the astrodynamics specialists to submit their research articles to this new journal. Currently, the scope of the journal includes, but is not limited to:Fundamental orbital dynamicsSpacecraft trajectory optimization and space mission designOrbit determination and prediction, autonomous orbital navigationSpacecraft attitude determination, control, and dynamicsGuidance and control of spacecraft and space robotsSpacecraft constellation design and formation flyingModelling, analysis, and optimization of innovative space systemsNovel concepts for space engineering and interdisciplinary applicationsThe effort of the Editorial Board will be ensuring the journal to publish novel researches that advance the field, and will provide authors with a productive, fair, and timely review experience. It is our sincere hope that all researchers in the field of astrodynamics will eagerly access this journal, Astrodynamics, as either authors or readers, making it an illustrious journal that will shape our future space explorations and discoveries.
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