N-body simulations find that primordial mass segregation imprints denser, unified tidal tails with bottom-heavy mass functions on star clusters, with effects strongest early and at small R_G but converging later.
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An intermediate-mass companion to Sgr A* plus resonant relaxation in a depleting gas disk can simultaneously produce the observed orbits of S-stars, clockwise disk stars, and off-disk stars within their 6-15 Myr lifetimes.
citing papers explorer
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The fingerprint of primordial mass segregation on the tidal tails of star clusters
N-body simulations find that primordial mass segregation imprints denser, unified tidal tails with bottom-heavy mass functions on star clusters, with effects strongest early and at small R_G but converging later.
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The complex kinematics of the young stars orbiting the supermassive black hole in the Galactic center can be explained by the presence of an intermediate mass companion of Sgr A$^\star$
An intermediate-mass companion to Sgr A* plus resonant relaxation in a depleting gas disk can simultaneously produce the observed orbits of S-stars, clockwise disk stars, and off-disk stars within their 6-15 Myr lifetimes.