Concurrent Formation of Carbon and Silicate Dust in Nova V1280 Sco

Abstract

We present infrared multi-epoch observations of the dust forming nova V1280 Sco over $\sim$2000 days from the outburst. The temporal evolution of the infrared spectral energy distributions at 1272, 1616 and 1947 days can be explained by the emissions produced by amorphous carbon dust of mass (6.6--8.7)$\times$10${}^{-8}$M${}_{\odot }$ with a representative grain size of 0.01$\mu$m and astronomical silicate dust of mass (3.4--4.3)$\times$10${}^{-7}$M${}_{\odot }$ with a representative grain size of 0.3--0.5$\mu$m. Both of these dust species travel farther away from the white dwarf without an apparent mass evolution throughout those later epochs. The dust formation scenario around V1280 Sco suggested from our analyses is that the amorphous carbon dust is formed in the nova ejecta followed by the formation of silicate dust in the expanding nova ejecta or as a result of the interaction between the nova wind and the circumstellar medium.

47 pages, 19 figures. Accepted for publication in the Astrophysical Journal on December 2, 2015

References in corpus (5)

• Dust and the type II-plateau supernova 2004et
• The unusual hydrocarbon emission from the early carbon star HD 100764: The connection between aromatics and aliphatics
• Near-Infrared Studies of V1280 Sco (Nova Scorpii 2007)
• The expanding dusty bipolar nebula around the nova V1280 Sco
• VLTI monitoring of the dust formation event of the Nova V1280 Sco

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• Mid-infrared Spectroscopic Observations of the Dust-forming Classical Nova V2676 Oph
• The Formation of Bimodal Dust Species in Nova Ejecta I: Chemical Conditions
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• Morpho-kinematic modeling of the expanding ejecta of the extremely slow nova V1280 Scorpii