Evans, A and Banerjee, DPK and Gehrz, RD and Joshi, V and Ashok, NM and Ribeiro, VARM and Darnley, MJ and Woodward, CE and Sand, D and Marion, GH and Diamond, TR and Eyres, SPS and Wagner, RM and Helton, LA and Starrfield, S and Shenoy, DP and Krautter, J and Vacca, WD and Rushton, MT (2017) Rise and fall of the dust shell of the classical nova V339 Delphini. Monthly Notices of the Royal Astronomical Society, 466 (4). pp. 4221-4238. ISSN 1365-2966

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Abstract

We present infrared spectroscopy of the classical nova V339 Delphini, obtained over a $\sim2$ year period. The infrared emission lines were initially symmetrical, with HWHM velocities of 525 km s$^{-1}$. In later ($t\gtrsim77$days, 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 $\sim$ day 34.75 at a condensation temperature of $1480\pm20$K, consistent with graphitic carbon. Thereafter the dust temperature declined with time as $T_{\rm d}\propto{t}^{-0.346}$, also consistent with graphitic carbon. The mass of dust initally rose, as a result of an increase in grain size and/or number, peaked at $\sim$ 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. An Appendix summarises Planck Means for carbon, and the determination of grain mass and radius for a carbon dust shell.

Item Type: Article © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society line:profiles; circumstellar matter; stars:individual:V339 Del; novae; cataclysmic variables; infrared:stars Q Science > QB AstronomyQ Science > QB Astronomy > QB799 Stars?? astro-ph.SR ?? Faculty of Natural Sciences > School of Physical and Geographical Sciences Author Symplectic 21 Mar 2017 15:55 21 Mar 2017 15:55 http://eprints.keele.ac.uk/id/eprint/3043