N-body simulations of ultra-faint dwarf galaxies without dark matter find a 3-billion-year quasi-stationary phase followed by mass segregation, with binaries causing substantial overestimates of velocity dispersion.
C., Askar, A., Kamlah, A
4 Pith papers cite this work. Polarity classification is still indexing.
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Simulations indicate stellar collisions dominate intermediate-mass black hole formation across cluster types, with potential to explain local globular cluster candidates and predict wandering IMBHs in Milky Way-like galaxies.
Direct N-body simulations independently confirm that preferential ejection of enriched RGB stars by an active black hole subsystem produces a transient overconcentration of pristine RGB stars in globular clusters that have lost substantial mass.
citing papers explorer
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The long-term evolution of Ultra Faint Dwarf Galaxies and observational implications
N-body simulations of ultra-faint dwarf galaxies without dark matter find a 3-billion-year quasi-stationary phase followed by mass segregation, with binaries causing substantial overestimates of velocity dispersion.
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Seeds to success: growing heavy black holes in dense star clusters
Simulations indicate stellar collisions dominate intermediate-mass black hole formation across cluster types, with potential to explain local globular cluster candidates and predict wandering IMBHs in Milky Way-like galaxies.
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Is the overconcentration of pristine populations in Galactic globular clusters real? An N-body approach to the problem
Direct N-body simulations independently confirm that preferential ejection of enriched RGB stars by an active black hole subsystem produces a transient overconcentration of pristine RGB stars in globular clusters that have lost substantial mass.
- Formation of intermediate-mass black holes in young massive clusters detected with JWST: analytic mass estimates