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 ∼ 2.4 kpc, reddening of E(B - V) ∼ 0.55, and WD mass of MWD = 0.82-0.96 M⊙. This suggests that an oxygen-neon WD lost a mass of more than ∼ 0.1 M⊙ since its birth. For V351 Pup, we obtained d ∼ 1.6 kpc, -Rfeti(BV) ∼ 0.45, and MWD = 0.98-1.1 M⊙. For V382 Vel, we obtained d ∼ 1.6 kpc, E(B-V) ∼ 0.15, and MWD = 1.13-1.28 M⊙. For V693 CrA, we obtained d ∼ 7.1 kpc, E (B - V) ∼ 0.05, and MWD = 1.151.25 M⊙. For V1974 Cyg, we obtained d ∼ 1.8 kpc, E (B - V) ∼ 0.30, and MWD = 0.951.1 M⊙. For comparison, we added the carbon-oxygen nova V1668 Cyg to our analysis and obtained d ∼ 5.4 kpc, E (B - V) ∼ 0.30, and MWD = 0.981.1 M⊙. 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 relation for these novae based on the universal decline law.
- novae, cataclysmic variables
- stars: individual (QU Vul, V351 Pup, V382 Vel, V693 CrA, V1974 Cyg)
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science