Carbon and silicate dust formation in V1280 Sco

11th Pacific Rim Conference on Stellar Astrophysics: Physics and Chemistry of the Late Stages of Stellar Evolution

物理学;天文学

Sakon, I.^1 ; Sako, S.^2 ; Oanaka, T.^1 ; Nozawa, T.^3 ; Kimura, Y.^4 ; Fujiyoshi, T.^5 ; Shimonishi, T.^6 ; Usui, F.^1 ; Takahashi, H.^2 ; Ohsawa, R.^2 ; Arai, A.^7 ; Uemura, M.^8 ; Nagayama, T.^9,10 ; Koo, B.-C.^11 ; Kozasa, T.^12

Department of Astronomy, Graduate Schools of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo

113-0033, Japan^1

Institute of Astronomy, University of Tokyo, 2-21-1 Ohsawa, Mitaka, Tokyo

181-0015, Japan^2

National Astronomical Observatory of Japan, Mitaka, Tokyo

181-8588, Japan^3

Institute of Low Temperature Science, Hokkaido University, Sapporo

060-0819, Japan^4

Subaru Telescope, National Astronomical Observatory of Japan, 650 North Aohoku Place, Hilo

HI

96720, United States^5

Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, Aramaki aza Aoba 6-3, Aoba-ku, Sendai

980-8578, Japan^6

Koyama Astronomical Observatory, Kyoto Sangyo University, Motoyama, Kamigamo, Kita-ku, Kyoto

603-8555, Japan^7

Hiroshima Astrophysical Science Center, Hiroshima University, Kagamiyama 1-3-1, Higashi-Hiroshima

739-8526, Japan^8

Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima

890-0065, Japan

(10) Department of Astrophysics, Nagoya University, Furo-cho, Chikusa-ku, Aichi, Nagoya

464-8602, Japan

(11) Department of Physics and Astronomy, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul

151-742, Korea, Republic of

(12) Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo

060-0810, Japan^9

关键词: Dust formation;    Grain size;    Infrared emissions;    Infrared spectral;    Temporal evolution;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/728/6/062006/pdf
DOI  :  10.1088/1742-6596/728/6/062006

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

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) × 10-8Mowith a representative grain size of 0.01 μm and astronomical silicate dust of mass (3.4-4.3) × 10-7Mowith 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.