Fig. 15.

image

Angular momentum and stellar mass of the tidal tails as a function of time for simulated star clusters. Left panel: evolution of the z component of the spin angular momentum, Lz, of the star cluster with time. We plot models M1, M2, and M3, which were evolved from the same initial conditions (see Table 2) but with different initial spin angular momenta (see Sect. 2.2). Model M4 considers the same MW potential as M1–M3 with the addition of lumps, and model M5 uses the MW potential from Irrgang et al. (2013). The Lz values are always computed within the tidal radius of the cluster. Right panel: mass outside of the tidal radius (Rt) of the cluster at a give time for the same models (M1, M2, and M3). The black lines are linear fits to the individual tracks and are used to compute the average mass-loss rate. The angular momentum of all our modelled clusters given by the motion in the Galaxy has a positive value.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.