Mass fraction of star‐forming gas for ﹩V_{\mathrm{vir}\,}=115﹩ km s⁻¹ (blue triangles) and ﹩V_{\mathrm{vir}\,}=500﹩ km s⁻¹ (red circles) progenitor merger remnants in simulations with gas fraction ﹩f_{\mathrm{gas}\,}=0.4﹩ as a function of time ﹩t-t_{\mathrm{disk}\,}﹩ since the disks first interact. The gas in the massive system is collisionally heated during the first passage and subsequently cannot cool and form stars, while gas in the small mass system can cool sufficiently to continue to form stars throughout the remainder of the merger.