Same as Figure 1, but including 75 nova models from Yaron et al. (2005), as triangles colored according to the mass of the WD in the nova binary. Larger mass WDs, as explained in the text, correlate with shorter t₂ . The masses of the WDs of the six faint, fast novae discovered by Kasliwal et al. (2011) (stars in the figure) are probably in the range of 1.0–1.25 M_⊙, while the three fastest novae detected in M87 by Shara et al. (2016) must contain WDs close to the Chandrasekhar mass.