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Fig. B.4.
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Osculating elements as a function of time for a binary with a stellar mass 50 M⊙ in orbit around a 106 M⊙ supermassive black hole in a a = 1 mpc orbit with an initial eccentricity e0 ∈ {0.5, 0.7, 0.9}. Only the argument of periastron, ω, shows a secular variation (bottom panel).
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