We present observations of the classical nova V1425 Aquilae (Nova Aquila 1995) with the Infrared Space Observatory's (ISO) Short Wavelength Spectrometer, the Isaac Newton Telescope's Intermediate Dispersion Spectrograph, and the International Ultraviolet Explorer's Short-Wavelength Primary Spectrograph. Analysis of He II (1640 Å) development constrains the white dwarf turnoff to ∼400 days after outburst. Photoionization modeling of the optical and ISO spectra obtained during the late nebular phase constrains the mass of the ejecta between 2.5-4.2 × 10-5 M⊙. This modeling also suggests C and O in the ejecta were enhanced by a factor of ∼9, and N was enhanced by a factor of ∼ 100 with respect to solar, while Ne was only slightly enhanced. Based upon these analyses, we determine that the white dwarf in the V1425 Aq1 system has a CO composition and is at a distance of 3.0 ± 0.4 kpc.
- Circumstellar matter
- Novae, cataclysmic variables
- Stars: individual (Nova Aquila 1995=V1425 Aquilae)