Abstract
Non-circular orbits are by no means rare, yet their eccentricities usually are small enough to be considered to first-order terms only.The angular velocitydv/dt and the radius vector R are then assumed to be constant for the comparatively short duration of each eclipse, providing a simple method to allow for the eccentricity e. The element ω is reckoned from the ascending node which each component passes 90° before undergoing eclipse.
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© 1978 D. Reidel Publishing Company, Dordrecht, Holland
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Heintz, W.D. (1978). Eccentric Orbits. In: Double Stars. Geophysics and Astrophysics Monographs, vol 15. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-9836-0_42
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DOI: https://doi.org/10.1007/978-94-009-9836-0_42
Publisher Name: Springer, Dordrecht
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