Abstract
Encke's method as modified by Potter to increase the accuracy of orbit computations of gravitationally interacting bodies is applied to the problem of relative motion of non-interacting space vehicles. This technique is then combined with a simple transformation of the independent variable to arrive at a system of equations from which the relative motion may be determined with increased precision.
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References
Battin, R.: 1965,Astronomical Guidance, McGraw Hill Co., New York, p. 216.
Eades, J. B.: 1973–75,Analytical Mechanics Associates Reports.
Eggleston, J. M.: 1965,NASA-TN D-1029.
Encke, J. F.: 1857,Berliner Jahrbuch.
Euler, L.: 1772,Theoria Motuum Lunae, Acad. Petropoli.
Nacozy, P.: 1973,Bull. of the Am. Astronomical Soc., Vol. 5, No. 1.
Stiefel, E. and Scheifele, G.: 1971,Linear and Regular Celestial Mechanics, Springer Publishing Company, New York.
Sundman, K.: 1912,Acta Math. 36, 105.
Szebehely, V.: 1976,Celestial Mechanics, in print.
Velez, C. E.: 1974,Celestial Mechanics, Vol. 10, No. 4, p. 405.
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Nacozy, P., Szebehely, V. The computation of relative motion with increased precision. Celestial Mechanics 13, 449–453 (1976). https://doi.org/10.1007/BF01229097
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DOI: https://doi.org/10.1007/BF01229097