On the Numerical Integration of the N-Body Problem for Star Clusters

Details On the Numerical Integration of the N-Body Problem for Star Clusters On the Numerical Integration of the N-Body Problem for Star Clusters

Sep 1972

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1972baas....4..423w&link_type=abstract

Bulletin of the American Astronomical Society 4, 423

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We describe a numerical procedure of integrating the equations of motion of the gravitational N-body problem, which has been successfully used for integrating systems with up to 500 stars (Aarseth, Wielen). The method uses polynomials which typically include the fifth time-derivative of the acceleration. The time step varies with time and differs from star to star. A discussion of the observed range of individual time steps indicates a large gain in computational efficiency by using individual time steps instead of integrating all the equations with the same step size

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