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

Abstract

We present infrared spectroscopy of the classical nova V339 Delphini, obtained over a $\sim 2$ year period. The infrared emission lines were initially symmetrical, with HWHM velocities of 525 km s${}^{-1}$. In later ($t\gtrsim 77$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 $1480\pm 20$K, consistent with graphitic carbon. Thereafter the dust temperature declined with time as $T_{\mathrm{d}}\propto t^{-0.346}$, 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.

arXiv commentAccepted by MNRAS on 19 December 2016. 19 pages

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