Origin of Dust around V1309 Sco

Abstract

The origin of dust grains in the interstellar medium is still open problem. \cite{Nicholls2013} found the presence of a significant amount of dust around V1309 Sco which maybe originate from the merger of a contact binary. We investigate the origin of dust around V1309 Sco, and suggest that these dust grains are efficiently produced in the binary-merger ejecta. By means of \emph{AGBDUST} code, we estimate that $\sim 5.2\times 10^{-4}{M}_{\odot }$ of dust grains are produced, and their radii are $\sim 10^{-5}$ cm. These dust grains mainly are composed of silicate and iron grains. Because the mass of the binary-merger ejecta is very small, the contribution of dust produced by binary-merger ejecta to the overall dust production in the interstellar medium is negligible. However, it is the most important that the discovery of a significant amount of dust around V1309 Sco offers a direct support for the idea---common-envelope ejecta provides an ideal environment for dust formation and growth. Therefore, we confirm that common-envelope ejecta can be important source of cosmic dust.

7 pages, 4 figures, Accepted for publication in the Astrophysical Journal

References in corpus (5)

• The Evolution of Dust in the Early Universe with Applications to the Galaxy SDSS J1148+5251
• Identification of the Long-Sought Common-Envelope Events
• The global gas and dust budget of the Small Magellanic Cloud
• The Dusty Aftermath of the V1309 Sco Binary Merger
• Dust Formation in the Ejecta of Common Envelope Systems

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• X-ray time delays from the Seyfert 2 galaxy IRAS 18325-5926
• The Formation of Bimodal Dust Species in Nova Ejecta I: Chemical Conditions
• The Formation of Bimodal Dust Species in Nova Ejecta