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 $\sim2$ 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.

Citation

(2017). Rise and fall of the dust shell of the classical nova V339 Delphini. Monthly Notices of the Royal Astronomical Society, 4221-4238. https://doi.org/10.1093/mnras/stw3334

• Acceptance Date: Dec 19, 2016
• Publication Date: Jan 13, 2017
• Journal: Monthly Notices of the Royal Astronomical Society
• Print ISSN: 0035-8711
• Publisher: Oxford University Press
• Pages: 4221-4238
• DOI: https://doi.org/10.1093/mnras/stw3334
• Keywords: line:profiles; circumstellar matter; stars:individual:V339 Del; novae; cataclysmic variables; infrared:stars
• Publisher URL: http://dx.doi.org/10.1093/mnras/stw3334