An efficient integrator for stellar dynamics in effective gravity fields based on the isochrone potential

Open Access

Fig. 2

Relative error in total energy as a function of time for the same orbit as in Fig. 1. The behaviour of two fourth-order integrators is shown: the Runge-Kutta method and the 𝒮𝒜ℬ𝒜₂ method using the isochrone splitting (see the labels). A constant time step δt = 2.5 is used for both integrators.

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