The enigmatic double-peaked stripped-envelope SN 2023aew
文献类型：期刊论文
| 作者 | Kangas, T.27,28; Kuncarayakti, H.27,28; Nagao, T.25,26,27; Kotak, R.27; Kankare, E.27; Fraser, M.24; Stevance, H.23; Mattila, S.22,27; Maeda, K.21; Stritzinger, M.20 |
| 刊名 | Astronomy and Astrophysics
 |
| 出版日期 | 2024-09-01 |
| 卷号 | 689 |
| 关键词 | accretion accretion disks stars: magnetars stars: mass loss supernovae: individual: SN 2023aew |
| ISSN号 | 0004-6361 |
| DOI | 10.1051/0004-6361/202449420 |
| 产权排序 | 第24完成单位 |
| 文献子类 | Journal article (JA) |
| 英文摘要 | We present optical and near-infrared photometry and spectroscopy of SN 2023aew and our findings on its remarkable properties. This event, initially resembling a Type IIb supernova (SN), rebrightens dramatically ~90 d after the first peak, at which time its spectrum transforms into that of a SN Ic. The slowly evolving spectrum specifically resembles a post-peak SN Ic with relatively low line velocities even during the second rise. The second peak, reached 119 d after the first peak, is both more luminous (Mr = -18.75±0.04 mag) and much broader than those of typical SNe Ic. Blackbody fits to SN 2023aew indicate that the photosphere shrinks almost throughout its observed evolution, and the second peak is caused by an increasing temperature. Bumps in the light curve after the second peak suggest interaction with circumstellar matter (CSM) or possibly accretion. We consider several scenarios for producing the unprecedented behavior of SN 2023aew. Two separate SNe, either unrelated or from the same binary system, require either an incredible coincidence or extreme fine-tuning. A pre-SN eruption followed by a SN requires an extremely powerful, SN-like eruption (consistent with ~1051 erg) and is also disfavored. We therefore consider only the first peak a true stellar explosion. The observed evolution is difficult to reproduce if the second peak is dominated by interaction with a distant CSM shell. A delayed internal heating mechanism is more likely, but emerging embedded interaction with a CSM disk should be accompanied by CSM lines in the spectrum, which are not observed, and is difficult to hide long enough. A magnetar central engine requires a delayed onset to explain the long time between the peaks. Delayed fallback accretion onto a black hole may present the most promising scenario, but we cannot definitively establish the power source. © The Authors 2024. |
| 学科主题 | 天文学 ; 恒星与银河系 |
| URL标识 | 查看原文 |
| 资助项目 | N/A |
| 语种 | 英语 |
| 资助机构 | N/A |
| 源URL | [http://ir.ynao.ac.cn/handle/114a53/27617]  |
| 专题 | 云南天文台_丽江天文观测站（南方基地） 云南天文台_中国科学院天体结构与演化重点实验室 |
| 作者单位 | 1.INAF - Osservatorio Astronomico di Brera, Via E. Bianchi 46 (LC), Merate, 23807, Italy 2.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile; 3.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, 650216, China; 4.International Centre of Supernovae, Yunnan Key Laboratory, Kunming, 650216, China; 5.Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, China; 6.Pondicherry University, Chinna Kalapet, Kalapet, Puducherry, 605014, India; 7.Indian Institute of Astrophysics, II Block, Koramangala, Bengaluru, Karnataka, 560034, India; 8.Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima, 739-8526, Japan; 9.Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, United Kingdom; 10.Department of Physics, University of Crete, Vasilika Bouton, Heraklion, 70013, Greece; |
| 推荐引用方式 GB/T 7714 | Kangas, T.,Kuncarayakti, H.,Nagao, T.,et al. The enigmatic double-peaked stripped-envelope SN 2023aew[J]. Astronomy and Astrophysics,2024,689. |
| APA | Kangas, T..,Kuncarayakti, H..,Nagao, T..,Kotak, R..,Kankare, E..,...&Reguitti, A..(2024).The enigmatic double-peaked stripped-envelope SN 2023aew.Astronomy and Astrophysics,689. |
| MLA | Kangas, T.,et al."The enigmatic double-peaked stripped-envelope SN 2023aew".Astronomy and Astrophysics 689(2024). |
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来源：云南天文台
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