Same as Figure 1, but including 75 nova models from Yaron et al. (2005) represented as triangles colored according to the total hydrogen-rich mass accreted onto the WD in the nova binary. The fastest novae (with smallest t2) have accreted the lowest mass hydrogen-rich envelopes—10−7–10−8 M⊙—while the slowest novae (largest t2) have accreted envelopes 1,000 to 10,000 times more massive. From this figure and Figure 2 it is clear that the total accreted envelope mass is as critical as a parameter as the WD mass in determining the peak luminosity and t2 of a nova.