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/987654321/101259
|
| 題名: | Superluminous supernovae from PESSTO |
| 作者: | 陳婷琬;Nicholl, M.;Smartt, S. J.;Jerkstrand, A.;Inserra, C.;Anderson, J. P.;Baltay, C.;Benetti, S.;Chen, T.-W.;Elias-Rosa, N.;Feindt, U.;Fraser, M.;Gal-Yam, A.;Hadjiyska, E.;Howell, D. A.;Kotak, R.;Lawrence, A.;Leloudas, G.;Margheim, S.;Mattila, S.;McCrum, M.;McKinnon, R.;Mead, A.;Nugent, P.;Rabinowitz, D.;Rest, A.;Smith, K. W.;Sollerman, J.;Sullivan, M.;Taddia, F.;Valenti, S.;Walker, E. S.;Young, D. R. |
| 貢獻者: | 理學院天文研究所 |
| 關鍵詞: | Astrophysics;Light;Luminosity;Radioactivity;Spectrum analysis;Supernovae;supernovae: general;supernovae: individual: LSQ12dlf;supernovae: individual: SN 2013dg;supernovae: individual: SSS120810:231802-560926;X-ray astronomy |
| 日期: | 2014-11-01 |
| 上傳時間: | 2026-04-21 14:28:35 (UTC+8) |
| 出版者: | Oxford University Press;London: Oxford University Press |
| 摘要: | 摘要： We present optical spectra and light curves for three hydrogen-poor superluminous supernovae followed by the Public ESO Spectroscopic Survey of Transient Objects (PESSTO). Time series spectroscopy from a few days after maximum light to 100 d later shows them to be fairly typical of this class, with spectra dominated by Ca ii, Mg ii, Fe ii, and Si ii, which evolve slowly over most of the post-peak photospheric phase. We determine bolometric light curves and apply simple fitting tools, based on the diffusion of energy input by magnetar spin-down, 56Ni decay, and collision of the ejecta with an opaque circumstellar shell. We investigate how the heterogeneous light curves of our sample (combined with others from the literature) can help to constrain the possible mechanisms behind these events. We have followed these events to beyond 100–200 d after peak, to disentangle host galaxy light from fading supernova flux and to differentiate between the models, which predict diverse behaviour at this phase. Models powered by radioactivity require unrealistic parameters to reproduce the observed light curves, as found by previous studies. Both magnetar heating and circumstellar interaction still appear to be viable candidates. A large diversity is emerging in observed tail-phase luminosities, with magnetar models failing in some cases to predict the rapid drop in flux. This would suggest either that magnetars are not responsible, or that the X-ray flux from the magnetar wind is not fully trapped. The light curve of one object shows a distinct rebrightening at around 100 d after maximum light. We argue that this could result either from multiple shells of circumstellar material, or from a magnetar ionization front breaking out of the ejecta.
其他題名： Mon. Not. R. Astron. Soc
出版者： London: Oxford University Press
出版日期： 2014-11-01
出處： Monthly notices of the Royal Astronomical Society, 2014-11, Vol.444 (3), p.2096-2113
資源來源： Alma/SFX Local Collection
版權： 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014
版權： Copyright Oxford University Press, UK Nov 1, 2014
識別號： ISSN: 0035-8711
識別號： ISSN: 1365-2966
識別號： EISSN: 1365-2966
識別號： DOI: 10.1093/mnras/stu1579 |
| 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 | 21 | 檢視/開啟 |
|
在NCUIR中所有的資料項目都受到原著作權保護.
|
