Extended Data Figure 5 : The dynamical model.

From: Rapidly rotating second-generation progenitors for the ‘blue hook’ stars of ω Centauri

Extended Data Figure 5

Two different cases of dynamical interactions are compared: either we make the hypothesis that the magnetic coupling of the disk is destroyed by one encounter with another star, at a distance entering the accretion disk (<100 au), or that three such encounters are necessary. a, A histogram of encounters versus time of detachment. b, Initial rotation period distribution employed in the two cases. c, Resulting distribution of the core mass increase, which is an initial parameter in the photometric simulation.