In Chap. 3, we know binaries already play a important role in stellar interactions. At an early stage, stellar interactions would disrupt most of soft binaries in a SC. However, the hard binaries would survive at this stage and continue with their further evolution, which would finally lead them to merge, resulting in BSS. Especially for binaries that contain massive stars, only a small fraction of them would evolve undisturbed towards their supernova explosion [172]. On the other hand, interacting massive binary and rotating stars would possibly contribute the enriched material to low-mass pre-main-sequence stars, which would lead the SCs to display a variety of metal abundance anomalies [173]. GCs, since they are extremely old, have a long time for stellar populations to evolve, which would lead to BSSs observable in photometry. In this Chapter, I present the research of BSSs in LMC GC Hodge 11, I show that the presence of BSSs in Hodge 11 is apparent, and their photometric features clearly indicate that they have different origins. We found that the BSSs originating from binary mergers and stellar collisions can be distinguished in their CMDs, which would offer us the rare opportunity to quantify the evolution of the cluster’s collisionally induced BSSs population.