The evolution of a star cluster in a pristine LCDM cusp background potential. The steep gravitational tides rapidly strip stars from the cluster, inhibiting its size growth and destroying it after 1.5Gyr.
The evolution of a star cluster in a fully cored background potential, where the star cluster is initially rotating with a velocity of 1.75km/s at the half-mass radius (5pc) and has a high ellipticity (e=0.30). The star cluster survives in the host potential for a Hubble time, and retains much of its initial ellipticity. This is because the weak gravitational tides in the core allow the star cluster to preserve its high angular momentum material.
The evolution of a star cluster in a fully cored background potential. The star cluster survives in the host potential for a Hubble time.
The evolution of a star cluster in a partially cored background potential. The gravitational tides encourage the formation of tidal tails, and the lowered background potential allows for a large cluster size as compared to a pristine LCDM cusp. After 1.25Gyr, the star cluster remains relatively large despite a high degree of tidal deformation.
