Tidal tails around globular clusters
M. Montuori (1), R. Capuzzo-Dolcetta (2), P. Di Matteo (3), P., Miocchi (2) ((1) CNR-INFM, Roma, Italy, (2) Dep. of Physics, La Sapienza, Univ. of Roma, Italy, (3) Obs. de Paris, LERMA, Paris, France)
TL;DR
This paper uses detailed N-body simulations to study how globular clusters develop tidal tails due to interactions with the Milky Way's bulge and disk, revealing their orientation and shape.
Contribution
It provides a realistic simulation-based analysis of tidal tail formation and morphology around globular clusters in the Milky Way.
Findings
Tidal tails form on opposite sides of clusters due to galactic interactions.
Tails' orientation and shape can be understood in a comoving frame.
Simulations match observed features of globular cluster tails.
Abstract
We present the results of detailed N-body simulations of clusters moving in a realistic Milky Way (MW) potential. The strong interaction with the bulge and the disk of the Galaxy leads to the formation of tidal tails, emanating from opposite sides of the cluster. Their orientation and morphology may be interpreted easily in terms of a comoving frame of coordinates.
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Taxonomy
TopicsCoastal and Marine Dynamics