We analyzed light curves of five neon novae , QU Vul , V351 Pup , V382 Vel , V693 CrA , and V1974 Cyg , and determined their white dwarf ( WD ) masses and distance moduli on the basis of theoretical light curves composed of free-free and photospheric emission .
For QU Vul , we obtained a distance of d \sim 2.4 kpc , reddening of E ( B - V ) \sim 0.55 , and WD mass of M _ { WD } = 0.82 – 0.96 ~ { } M _ { \sun } .
This suggests that an oxygen-neon WD lost a mass of more than \sim 0.1 ~ { } M _ { \sun } since its birth .
For V351 Pup , we obtained d \sim 5.5 kpc , E ( B - V ) \sim 0.45 , and M _ { WD } = 0.98 – 1.1 ~ { } M _ { \sun } .
For V382 Vel , we obtained d \sim 1.6 kpc , E ( B - V ) \sim 0.15 , and M _ { WD } = 1.13 – 1.28 ~ { } M _ { \sun } .
For V693 CrA , we obtained d \sim 7.1 kpc , E ( B - V ) \sim 0.05 , and M _ { WD } = 1.15 – 1.25 ~ { } M _ { \sun } .
For V1974 Cyg , we obtained d \sim 1.8 kpc , E ( B - V ) \sim 0.30 , and M _ { WD } = 0.95 – 1.1 ~ { } M _ { \sun } .
For comparison , we added the carbon-oxygen nova V1668 Cyg to our analysis and obtained d \sim 5.4 kpc , E ( B - V ) \sim 0.30 , and M _ { WD } = 0.98 – 1.1 ~ { } M _ { \sun } .
In QU Vul , photospheric emission contributes 0.4 – 0.8 mag at most to the optical light curve compared with free-free emission only .
In V351 Pup and V1974 Cyg , photospheric emission contributes very little ( 0.2 – 0.4 mag at most ) to the optical light curve .
In V382 Vel and V693 CrA , free-free emission dominates the continuum spectra , and photospheric emission does not contribute to the optical magnitudes .
We also discuss the Maximum Magnitude versus Rate of Decline ( MMRD ) relation for these novae based on the universal decline law .