@article{b6081cae54ee4d819eb862be9c85bfb7,
title = "Rise and fall of the dust shell of the classical nova V339 Delphini",
abstract = "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.",
keywords = "Cataclysmic variables, Circumstellar matter, Infrared: stars, Line: profiles, Novae, Stars: individual: V339 Del",
author = "A. Evans and Banerjee, {D. P.K.} and Gehrz, {R. D.} and V. Joshi and Ashok, {N. M.} and Ribeiro, {V. A.R.M.} and Darnley, {M. J.} and Woodward, {C. E.} and D. Sand and Marion, {G. H.} and Diamond, {T. R.} and Eyres, {S. P.S.} and Wagner, {R. M.} and Helton, {L. A.} and S. Starrfield and Shenoy, {D. P.} and J. Krautter and Vacca, {W. D.} and Rushton, {M. T.}",
note = "Funding Information: We thank Dr Kim Page for valuable information about the early X-ray emission of V339 Del, and the British Astronomical Association, The Astronomer magazine and the AAVSO for providing its visual light curve. We also appreciate the referee's supportive comments on this paper. RDG acknowledges support from the National Aeronautics and Space Administration (NASA) and the United States Air Force. VARMR acknowledges financial support from the Radboud Excellence Initiative. CEW acknowledges partial support from NASA (HST-GO-13828.008-A). SS gratefully acknowledges partial support from both NASA and NSF grants to ASU. The research work at the Physical Research Laboratory is supported by the Department of Space, Government of India. DS is a visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with NASA. Funding Information: RDG acknowledges support from the National Aeronautics and Space Administration (NASA) and the United States Air Force. VARMR acknowledges financial support from the Radboud Excellence Initiative. CEW acknowledges partial support from NASA (HST-GO-13828.008-A). SS gratefully acknowledges partial support from both NASA and NSF grants to ASU. The research work at the Physical Research Laboratory is supported by the Department of Space, Government of India. DS is a visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with NASA. Publisher Copyright: {\textcopyright} 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society",
year = "2017",
month = may,
day = "1",
doi = "10.1093/mnras/stw3334",
language = "English (US)",
volume = "466",
pages = "4221--4238",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",
}