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Gravitation and Cosmology

, Volume 23, Issue 4, pp 294–299 | Cite as

Quasi-elliptic trajectories in the gravitational field of a rotating star

Article

Abstract

A detailed derivation is given of formulas describing the trajectory of a test body moving closely to the ecliptic plane of a rotating star whose gravitational field is modeled by the Kerr metric. It is found that the quasi-elliptic orbit parameters and the revolution period noticeably change (as compared to the classical case), and an additional orbit precession emerges, though four orders of magnitude weaker than that of the Einstein-Schwarzschild case.

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References

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    A. Einstein, “Erklärung der Perihelbewegung des Merkur aus der allgemeinen Realtivitatstheorie,” Koniglich Preussische Akademie der Wissenschaften Sitzungsberichte (Berlin, 1915), pp. 831–839.Google Scholar
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    H. Stephani, D. Kramer, M. MacCallum, C. Hoenselaers, and E. Herlt, Exact Solutions of Equations of General Theory of Relativity (Cambridge University Press, Cambridge, 2003), p. 205.MATHGoogle Scholar

Copyright information

© Pleiades Publishing, Ltd. 2017

Authors and Affiliations

  1. 1.Institute of Gravitation and CosmologyRUDN UniversityMoscowRussia

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