Infrared observations of dust formation and coronal emission in nova aquilae 1995

C. G. Mason, R. D. Gehrz, Charles E. Woodward, J. B. Smiloerrz, Matthew A. Greenhouse, T. L. Hayward, J. R. Houck

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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 languageEnglish (US)
Pages (from-to)577-582
Number of pages6
JournalAstrophysical Journal
Issue number1 PART I
StatePublished - Jan 1 1996


  • Dust, extinction - Infrared
  • Individual (nova aquilae 1995)
  • Stars - Novae, cataclysmic variables stars


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