We report 1.25-18.5 μm infrared spectrophotometric measurements of Nova Aquilae 1995. Photometric measurements were obtained over a four month period following the formation of an optically thin dust shell. Hydrogen and helium emission lines were evident throughout this period, along with strong near-infrared coronal line emission that appeared approximately 120 days after outburst. Both the photometric and the spectroscopic data suggest that the ejecta were clumpy, and that they contained both a dust component and a hot gas component. The outflow velocity of the ionized ejecta was observed to be ∼ 1365-1600 km s-1 (FWHM), and no appreciable deceleration of the ejecta was observed over the duration of these observations. Based on a Mv-t2 light decline relationship, we calculate a distance of ∼ 3.6-4.8 kpc.
|Original language||English (US)|
|Number of pages||6|
|Issue number||1 PART I|
|State||Published - Jan 1 1996|
- Dust, extinction - Infrared
- Individual (nova aquilae 1995)
- Stars - Novae, cataclysmic variables stars