Mathieu Renzo, University of Amsterdam - 15.07.19
Most massive stars are born in clusters and typically have a binary companion. However, a significant fraction of massive stars is observed in relative isolation, moving at large velocities, and typically single. Because of their motion, the region of the host galaxy influenced by their chemical, mechanical, and radiative feedback increases significantly. The large velocities of these stars are the result either of gravitational N-body interactions in a cluster or of the explosion of a companion star in a binary. Both mechanism are competing in nature. In this talk, I will compare these two ejection mechanism, and outline how the kinematics of massive stars as observed by Gaia can be used to learn about the early dynamics in a dense stellar clusters or to constrain the explosion physics of core-collapse supernovae, and in particular the natal kick imparted to newly formed black holes.