Carbon and silicate dust formation in V1280 Sco

I. Sakon, S. Sako, T. Oanaka, T. Nozawa, Y. Kimura, T. Fujiyoshi, T. Shimonishi, F. Usui, H. Takahashi, R. Ohsawa, A. Arai, M. Uemura, T. Nagayama, B. C. Koo, T. Kozasa

Research output: Contribution to journalConference articlepeer-review


This study investigates the temporal evolution of the infrared emission from the dusty nova V1280 Sco over 2000 days from the outburst. We have revealed that the infrared spectral energy distributions at 1272, 1616 and 1947 days are explained by the emissions produced by amorphous carbon dust of mass (6.6-8.7) × 10-8 M with a representative grain size of 0.01 μm and astronomical silicate dust of mass (3.4-4.3) × 10-7 M with a representative grain size of 0.3-0.5 μm. Both of carbon and silicate dust travel farther away from the white dwarf without an apparent mass evolution throughout those later epochs.

Original languageEnglish
Article number062006
JournalJournal of Physics: Conference Series
Issue number6
Publication statusPublished - 2016 Aug 8
Event11th Pacific Rim Conference on Stellar Astrophysics: Physics and Chemistry of the Late Stages of Stellar Evolution - Hong Kong, China
Duration: 2015 Dec 142015 Dec 17

ASJC Scopus subject areas

  • Physics and Astronomy(all)


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