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Motion in the ER3BP with an oblate primary and a triaxial stellar companion

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Abstract

The triangular points of the elliptic restricted three-body problem under an oblate primary and a triaxial and radiating secondary are investigated. Their positions and stability are found to be affected by the eccentricity, semi-major axis, oblateness, triaxiality and radiation pressure. Using Low and High Mass X-ray binaries (LMXB and HMXB), we highlight the effects of the said parameters on the positions of the triangular points of PSR J1903+0327, CEN X-4 and RXJ 04050.01.5658. The triangular points are found to be stable for \(0 < \mu < \mu_{C}\); where \(\mu\) is the mass ratio \(( \mu \le \frac{1}{2} )\). The effects of the parameters on the regions of stability are shown graphically within the stable interval, highlighting their destabilizing tendencies.

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  1. Department of Mathematics, Faculty of Science, Ahmadu Bello University Zaria, Zaria, Nigeria

    Aishetu Umar & Aminu Abubakar Hussain

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  1. Aishetu Umar
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Correspondence to Aminu Abubakar Hussain.

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Umar, A., Hussain, A.A. Motion in the ER3BP with an oblate primary and a triaxial stellar companion. Astrophys Space Sci 361, 344 (2016). https://doi.org/10.1007/s10509-016-2918-6

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