Massive black hole formation in Population III star clusters

Open Access

Fig. 7

Root-mean-square velocity of stars in the cluster core as a function of time for all the models with ${\dot{ρ}}_{0} = 0.142 M_{⊙} y r^{- 1} p c^{- 3}$ $\dot{\rho}_0=0.142$~M$_\odot$~yr$^{-1}$~pc$^{-3}$ . The rate for the increase in v_rms,core correlates with the SF efficiency. We also note that after SF ceases at 0.5 Myr for model E6 (rapid SF), the rate at which v_rms,core increases is lower.

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