資料載入中.....
|
請使用永久網址來引用或連結此文件:
https://ir.lib.ncu.edu.tw/handle/987654321/101535
|
| 題名: | Nebular spectra and abundance tomography of the Type Ia supernova SN 2011fe: A normal SN Ia with a stable Fe core |
| 作者: | 潘彥丞;Mazzali, P. A.;Sullivan, M.;Filippenko, A. V.;Garnavich, P. M.;Clubb, K. I.;Maguire, K.;Pan, Y.-C.;Shappee, B.;Silverman, J. M.;Benetti, S.;Hachinger, S.;Nomoto, K.;Pian, E. |
| 貢獻者: | 理學院天文研究所 |
| 關鍵詞: | Abundance;Astronomy;Density;Heating;Iron;Light curve;Neutrons;Spectra;Supernovae;Supernovas;Symbols;Tomography |
| 日期: | 2015-07-01 |
| 上傳時間: | 2026-04-21 14:37:15 (UTC+8) |
| 出版者: | Oxford University Press;London: Oxford University Press |
| 摘要: | 摘要： A series of optical and one near-infrared nebular spectra covering the first year of the Type Ia supernova SN 2011fe are presented and modelled. The density profile that proved best for the early optical/ultraviolet spectra, ‘ρ-11fe’, was extended to lower velocities to include the regions that emit at nebular epochs. Model ρ-11fe is intermediate between the fast deflagration model W7 and a low-energy delayed-detonation. Good fits to the nebular spectra are obtained if the innermost ejecta are dominated by neutron-rich, stable Fe-group species, which contribute to cooling but not to heating. The correct thermal balance can thus be reached for the strongest [Fe ii] and [Fe iii] lines to be reproduced with the observed ratio. The 56Ni mass thus obtained is ∼0.47 ± 0.05 M⊙. The bulk of 56Ni has an outermost velocity of ∼8500 km s−1. The mass of stable iron is ∼0.23 ± 0.03 M⊙. Stable Ni has low abundance, ∼10−2 M⊙. This is sufficient to reproduce an observed emission line near 7400 Å. A sub-Chandrasekhar explosion model with mass 1.02 M⊙ and no central stable Fe does not reproduce the observed line ratios. A mock model where neutron-rich Fe-group species are located above 56Ni following recent suggestions is also shown to yield spectra that are less compatible with the observations. The densities and abundances in the inner layers obtained from the nebular analysis, combined with those of the outer layers previously obtained, are used to compute a synthetic bolometric light curve, which compares favourably with the light curve of SN 2011fe.
其他題名： Mon. Not. R. Astron. Soc
出版者： London: Oxford University Press
出版日期： 2015-07-01
出處： Monthly notices of the Royal Astronomical Society, 2015-07, Vol.450 (3), p.2631-2643
資源來源： Alma/SFX Local Collection
版權： 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2015
版權： Copyright Oxford University Press, UK Jul 1, 2015
識別號： ISSN: 0035-8711
識別號： ISSN: 1365-8711
識別號： ISSN: 1365-2966
識別號： EISSN: 1365-2966
識別號： DOI: 10.1093/mnras/stv761 |
| 顯示於類別: | [天文研究所] 期刊論文
|
文件中的檔案:
| 檔案 |
描述 |
大小 | 格式 | 瀏覽次數 |
|---|
| index.html | | 0Kb | HTML | 43 | 檢視/開啟 |
|
在NCUIR中所有的資料項目都受到原著作權保護.
|
