Rise and fall of the dust shell of the classical nova V339 Delphini

A. Evans, D. P.K. Banerjee, R. D. Gehrz, V. Joshi, N. M. Ashok, V. A.R.M. Ribeiro, M. J. Darnley, C. E. Woodward, D. Sand, G. H. Marion, T. R. Diamond, S. P.S. Eyres, R. M. Wagner, L. A. Helton, S. Starrfield, D. P. Shenoy, J. Krautter, W. D. Vacca, M. T. Rushton

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23 Scopus citations


We present infrared spectroscopy of the classical nova V339 Del, obtained over an ∼2-yr period. The infrared emission lines were initially symmetrical, with half width half-maximum velocities of 525 km s−1. In later (t ≳ 77 d, where t is the time from outburst) spectra, however, the lines displayed a distinct asymmetry, with a much stronger blue wing, possibly due to obscuration of the receding component by dust. Dust formation commenced at approximately day 34.75 at a condensation temperature of 1480 ± 20 K, consistent with graphitic carbon. Thereafter, the dust temperature declined with time as Td ∝ t−0.346, also consistent with graphitic carbon. The mass of dust initially rose, as a result of an increase in grain size and/or number, peaked at approximately day 100, and then declined precipitously. This decline was most likely caused by grain shattering due to electrostatic stress after the dust was exposed to X-radiation. The appendix summarizes Planck means for carbon and the determination of grain mass and radius for a carbon dust shell.

Original languageEnglish (US)
Pages (from-to)4221-4238
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Issue number4
StatePublished - May 1 2017

Bibliographical note

Publisher Copyright:
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society


  • Cataclysmic variables
  • Circumstellar matter
  • Infrared: stars
  • Line: profiles
  • Novae
  • Stars: individual: V339 Del


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