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Figure 5: Lagrange radii indicating the evolution of a Plummer model globular cluster for an N-body
simulation and a Monte Carlo simulation. The radii correspond to radii containing 0.35, 1, 3.5, 5, 7,
10, 14, 20, 30, 40, 50, 60, 70, and 80% of the total mass. Image reproduced by permission from Joshi
et al. [253], copyright by IOP.
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Matthew J. Benacquista and Jonathan M. B. Downing, "Relativistic Binaries in Globular Clusters",
Living Rev. Relativity, 16 (2013), 4, doi:10.12942/lrr-2013-4, URL (accessed <date>): http://www.livingreviews.org/lrr-2013-4.
This work is licensed under a Creative Commons License.
© The author(s), except where otherwise noted.
Living Rev. Relativity, 16 (2013), 4, doi:10.12942/lrr-2013-4, URL (accessed <date>): http://www.livingreviews.org/lrr-2013-4.
This work is licensed under a Creative Commons License.
© The author(s), except where otherwise noted.