Reconstructing the Initial Relaxation Time of Young Star Clusters in the Large Magellanic Cloud

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dc.creatorZwart, Simon F. Portegies
dc.creatorChen, Hui-Chen
dc.date2006-10-23
dc.date.accessioned2026-07-07T07:27:04Z
dc.date.available2026-07-07T07:27:04Z
dc.descriptionWe reconstruct the initial two-body relaxation time at the half mass radius for a sample of young $\aplt 300$ Myr star clusters in the large Magellanic cloud. We achieve this by simulating star clusters with 12288 to 131072 stars using direct $N$-body integration. The equations of motion of all stars are calculated with high precision direct $N$-body simulations which include the effects of the evolution of single stars and binaries. We find that the initial relaxation times of the sample of observed clusters in the large Magellanic cloud ranges from about 200 Myr to about 2 Gyr. The reconstructed initial half-mass relaxation times for these clusters has a much narrower distribution than the currently observed distribution, which ranges over more than two orders of magnitude.
dc.descriptionTo appear in ``Mass loss from stars and the evolution of stellar clusters''. Proc. of a workshop held in honour of H.J.G.L.M. Lamers, Lunteren, The Netherlands. Eds. A. de Koter, L. Smith and R. Waters (San Francisco: ASP)
dc.identifierhttps://arxiv.org/abs/astro-ph/0610659
dc.identifierhttp://arxiv.org/abs/astro-ph/0610659
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/117254
dc.subjectAstrophysics
dc.titleReconstructing the Initial Relaxation Time of Young Star Clusters in the Large Magellanic Cloud
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