%0 Generic %1 Smith2011 %A Smith, R. %A Slater, R. %A Fellhauer, M. %A Goodwin, S. %A Assmann, P. %D 2011 %K cluster formation relaxation star %T Formation rates of star clusters in the hierarchical merging scenario %U http://arxiv.org/abs/1105.1953 %X Stars form with a complex and highly structured distribution. For a smooth star cluster to form from these initial conditions, the star cluster must erase this substructure. We study how substructure is removed using N-body simulations that realistically handle two-body relaxation. In contrast to previous studies, we find that hierarchical cluster formation occurs chiefly as a result of scattering of stars out of clumps, and not through clump merging. Two-body relaxation, in particular within the body of a clump, can significantly increase the rate at which substructure is erased beyond that of clump-merging alone. Hence the relaxation time of individual clumps is a key parameter controlling the rate at which smooth, spherical star clusters can form. The initial virial ratio of the clumps is an additional key parameter controlling the formation rate of a cluster. Reducing the initial virial ratio causes a star cluster to lose its substructure more rapidly.

@misc{Smith2011, abstract = { Stars form with a complex and highly structured distribution. For a smooth star cluster to form from these initial conditions, the star cluster must erase this substructure. We study how substructure is removed using N-body simulations that realistically handle two-body relaxation. In contrast to previous studies, we find that hierarchical cluster formation occurs chiefly as a result of scattering of stars out of clumps, and not through clump merging. Two-body relaxation, in particular within the body of a clump, can significantly increase the rate at which substructure is erased beyond that of clump-merging alone. Hence the relaxation time of individual clumps is a key parameter controlling the rate at which smooth, spherical star clusters can form. The initial virial ratio of the clumps is an additional key parameter controlling the formation rate of a cluster. Reducing the initial virial ratio causes a star cluster to lose its substructure more rapidly. }, added-at = {2011-05-11T20:02:47.000+0200}, author = {Smith, R. and Slater, R. and Fellhauer, M. and Goodwin, S. and Assmann, P.}, biburl = {https://www.bibsonomy.org/bibtex/24973ba929d7abbaf96bca5d3ac976ade/miki}, description = {[1105.1953] Formation rates of star clusters in the hierarchical merging scenario}, interhash = {9b4630c242648c7a2afe614f7ae0c411}, intrahash = {4973ba929d7abbaf96bca5d3ac976ade}, keywords = {cluster formation relaxation star}, note = {cite arxiv:1105.1953 Comment: 9 pages, 5 figures}, timestamp = {2011-05-11T20:02:47.000+0200}, title = {Formation rates of star clusters in the hierarchical merging scenario}, url = {http://arxiv.org/abs/1105.1953}, year = 2011 }