Application of binary pulsars to axisymmetric bodies in the Elliptic R3BP

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• 作者：Jagadish Singh (1)
  Aishetu Umar (1)
  
• 关键词：Celestial mechanics ; Axisymmetric ER3BP ; Double pulsars
• 刊名：Astrophysics and Space Science
• 出版年：2013
• 出版时间：December 2013
• 年：2013
• 卷：348
• 期：2
• 页码：393-402
• 全文大小：
• 作者单位：Jagadish Singh (1)
  Aishetu Umar (1)
  
  1. Department of Mathematics, Faculty of Science, Ahmadu Bello University Zaria, Zaria, Nigeria
  
• ISSN：1572-946X

文摘

Binary systems hosting astrophysical compact objects such as white dwarfs and/or neutron stars provide excellent test beds for studying the impact of the oblateness of the main bodies in the restricted three-body problem (R3BP). The case is investigated when the primary bodies are non-luminous, non-spherical (oblate) bodies and the third body of infinitesimal mass is also an oblate spheroid. The existence of extra solar planets orbiting these systems constitutes a three-body problem which makes them excellent models for this axisymmetric ER3BP. The positions of the equilibrium points are affected by the oblateness parameters of the three-bodies; this is shown for double neutron star binaries. The triangular points are stable for 0<μ<μ c ; where μ is the mass ratio (μ≤1/2) and μ c is the critical mass value influenced by the eccentricity, semi major axis and oblateness factors. The size of the region of stability increases with decreasing values of the oblateness. The oblateness of the system’s bodies does not affect the nature of the stability of the collinear points since they remain unstable. Due to the almost equal masses of the primaries, our study shows that even the triangular points of these systems are unstable.