Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.
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N-body simulations show wide binaries disrupt rapidly in the first 10 Myr due to high-density encounters, with semi-analytical models matching the evolution and identifying young low-density clusters as optimal detection sites.
GaiaNIR retains sensitivity to extended dark matter halos in globular clusters under strong extinction while Gaia degrades, enabling studies in obscured regions.
N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.
citing papers explorer
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Simulating Star Formation and Star Cluster Assembly in the Aquila Rift Using Archival Observations
Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.
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Formation and disruption of wide binaries in star clusters revealed by N-body simulations
N-body simulations show wide binaries disrupt rapidly in the first 10 Myr due to high-density encounters, with semi-analytical models matching the evolution and identifying young low-density clusters as optimal detection sites.
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From Gaia to GaiaNIR: I. Probing dark matter halos in globular clusters
GaiaNIR retains sensitivity to extended dark matter halos in globular clusters under strong extinction while Gaia degrades, enabling studies in obscured regions.
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Dynamical evolution of Milky Way globular clusters on the cosmological timescale II. Terzan 2, 4, and 5 mass loss and collision tracking
N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.