Dynamic evolution of the star system from Fleming et al. (2018), influenced by different initial Q factors usingthe CPL model. Redder curves represent low initial Q values, whilebluer curves represent higher Q values. We used the CPL model along with dynamic radius of gyration. Top: binaries’ dynamic stability limit time evolutions, a_crit. Middle: orbital period of the secondary star. Bottom: eccentricity of secondary star. The approximate runtime was 15 min. github.com: cbp_dynamic_stability/Qfactors/