Stability of orbits near large mass ratio binary systems

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• 作者：Natasha Bosanac (1)
  Kathleen C. Howell (1)
  Ephraim Fischbach (2)
  
  1. Purdue University ; 701 W. Stadium Ave. ; West Lafayette ; IN ; 47907 ; USA
  2. Purdue University ; 525 Northwestern Ave. ; West Lafayette ; IN ; 47907 ; USA
  
• 关键词：Circular restricted three ; body problem ; Stability analysis ; Periodic orbits ; Binary star systems ; Pulsar PSR B1620 ; 26 ; Exoplanets ; Planets in binaries ; Bifurcations
• 刊名：Celestial Mechanics & Dynamical Astronomy
• 出版年：2015
• 出版时间：May 2015
• 年：2015
• 卷：122
• 期：1
• 页码：27-52
• 全文大小：2,607 KB
• 参考文献：1. Benest, D (1977) Effects of the mass ratio on the existence of retrograde satellites in the circular restricted problem: IV. Three-dimensional stability of plane periodic orbits. Astron. Astrophys. 54: pp. 563-568
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  3. Bosanac, N., Howell, K.C., Fischbach, E.: Exploring the impact of a three-body interaction added to the gravitational potential function in the restricted three-body problem. In: 23rd AAS/AIAA Space Flight Mechanics Meeting, February 2013, Hawaii (2013)
  4. Bosanac, N., Howell, K.C., Fischbach, E.: Stability of orbits near large mass ratio binary systems. In: 2nd IAA Conference on Dynamics and Control of Space Systems, March 2014, Rome, Italy (2014)
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  16. Szebehely, V (1967) Theory of Orbits: The Restricted Problem of Three Bodies. Academic Press, London
  
• 刊物类别：Physics and Astronomy
• 刊物主题：Physics
  Astronomy
  Mathematics
  
• 出版者：Springer Netherlands
• ISSN：1572-9478

文摘

With improved observational capabilities and techniques, an increasing number of exoplanets have been discovered to orbit in the vicinity of binary star systems. In this investigation, periodic motions near a large mass ratio binary are explored within the context of the circular restricted three-body problem. Specifically, stability analysis is used to explore the effect of the mass ratio on the structure of families of periodic orbits. Such analysis is useful in a variety of applications, including the determination of potentially stable exoplanet motions near a binary star.