| The enigmatic double-peaked stripped-envelope SN 2023aew | |
Kangas, T.1,2; Kuncarayakti, H.1,2; Nagao, T.2,3,4; Kotak, R.2; Kankare, E.2; Fraser, M.5; Stevance, H.6; Mattila, S.2,7; Maeda, K.8; Stritzinger, M.9; Lundqvist, P.10; Elias-Rosa, N.11,12; Ferrari, L.13,14; Folatelli, G.13,14,15; Frohmaier, C.16; Galbany, L.12,17; Kawabata, M.18; Koutsiona, E.19; Bravo, T. E.12,17; Piscarreta, L.12,17; Pursiainen, M.20; Singh, A.21; Taguchi, K.8; Teja, R. S.22,23; Valerin, G.11; Pastorello, A.11; Benetti, S.11; Cai YZ(蔡永志)24,25,26 ; Charalampopoulos, P.2; Gutiérrez, C. P.12,17; Kravtsov, T.2,27; Reguitti, A.11,28
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| 发表期刊 | Astronomy and Astrophysics
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| 2024-09-01 | |
| 卷号 | 689 |
| DOI | 10.1051/0004-6361/202449420 |
| 产权排序 | 第24完成单位 |
| 收录类别 | EI |
| 关键词 | accretion accretion disks stars: magnetars stars: mass loss supernovae: individual: SN 2023aew |
| 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. |
| 资助项目 | N/A |
| 项目资助者 | N/A |
| 语种 | 英语 |
| 学科领域 | 天文学 ; 恒星与银河系 |
| 文章类型 | Journal article (JA) |
| ISSN | 0004-6361 |
| URL | 查看原文 |
| EI入藏号 | 20243817078426 |
| EI主题词 | Supernovae |
| EI分类号 | 1102.3.1 - 1301.1.3.1 - 1302.1.2 - 714.2 Semiconductor Devices and Integrated Circuits |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/27617 |
| 专题 | 南方基地 中国科学院天体结构与演化重点实验室 |
| 作者单位 | 1.Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Turku, 20014, Finland; 2.Department of Physics and Astronomy, University of Turku, Turku, 20014, Finland; 3.Aalto University Metsähovi Radio Observatory, Metsähovintie 114, Kylmälä, 02540, Finland; 4.Aalto University Department of Electronics and Nanoengineering, PO Box 15500, Aalto, 00076, Finland; 5.School of Physics, University College Dublin, L.M.I. Main Building, Beech Hill Road, Dublin, D04 P7W1, Ireland; 6.Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, United Kingdom; 7.School of Sciences, European University Cyprus, Diogenes Street, Engomi, Nicosia, 1516, Cyprus; 8.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan; 9.Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C, 8000, Denmark; 10.Oskar Klein Centre, Department of Astronomy, Stockholm University, Albanova University Centre, Stockholm, 106 91, Sweden; 11.INAF - Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, 35122, Italy; 12.Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans s/n, Barcelona, 08193, Spain; 13.Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, La Plata, B1900FWA, Argentina; 14.Instituto de Astrofísica de La Plata (IALP), CCT-CONICET-UNLP, Paseo del Bosque S/N, La Plata, B1900FWA, Argentina; 15.Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba, 277-8583, Japan; 16.School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, United Kingdom; 17.Institut d'Estudis Espacials de Catalunya (IEEC), Gran Capitá, 2-4, Edifici Nexus, Desp. 201, Barcelona, 08034, Spain; 18.Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo-cho, Sayo, Hyogo, 679-5313, Japan; 19.Department of Physics, University of Crete, Vasilika Bouton, Heraklion, 70013, Greece; 20.Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, United Kingdom; 21.Hiroshima Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima, 739-8526, Japan; 22.Indian Institute of Astrophysics, II Block, Koramangala, Bengaluru, Karnataka, 560034, India; 23.Pondicherry University, Chinna Kalapet, Kalapet, Puducherry, 605014, India; 24.Yunnan Observatories, Chinese Academy of Sciences, Kunming, 650216, China; 25.International Centre of Supernovae, Yunnan Key Laboratory, Kunming, 650216, China; 26.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, 650216, China; 27.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile; 28.INAF - Osservatorio Astronomico di Brera, Via E. Bianchi 46 (LC), Merate, 23807, Italy |
| 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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