The enigmatic double-peaked stripped-envelope SN 2023aew

doi:10.1051/0004-6361/202449420

YNAO OpenIR > 南方基地

	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
发表期刊	ASTRONOMY & ASTROPHYSICS
	2024-09-13
卷号	689
DOI	10.1051/0004-6361/202449420
产权排序	第24完成单位
收录类别	SCI ; 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 similar to 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 (M-r = -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 similar to 10(51) 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.
资助项目	Research Council of Finland[324504]; Research Council of Finland[328898]; Research Council of Finland[353019]; Research Council of Finland[340613]; Research Council of Finland[350458]; Royal Society - Science Foundation Ireland University Research Fellowship; Eric and Wendy Schmidt A.I. in Science Fellowship; JSPS KAKENHI[JP20H04737]; JSPS Open Partnership Bilateral Joint Research Project between Japan and Finland - Independent Research Fund Denmark (IRFD)[JPJSBP120229923]; Secretary of Universities and Research (Government of Catalonia); Horizon 2020 Research and Innovation Programme of the European Union under the Marie Sklodowska-Curie; Beatriu de Pinos[2021 BP 00168]; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI)[PID2020-115253GA-I00]; HOSTFLOWS project; Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; National Natural Science Foundation of China (NSFC)[12303054]; Yunnan Fundamental Research Projects[202401AU070063]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; UK Research and Innovation Fellowship[MR/T020784/1]; PRIN-INAF; MIUR, PRIN[20179ZF5KS]; INAF GRAWITA Large Program Grant; ESA Gaia, DPAC; Photometric Science Alerts Team; East Asian Observatory; Finland and Norway; University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias; Instituto de Astrofisica de Andalucia (IAA); University of Copenhagen and NOT; OPTICON[22A/012]; European Union[101004719]; Indian Institute of Astrophysics (IIA); Indian Institute of Technology Bombay (IITB); Indo-US Science and Technology Forum; Science and Engineering Research Board, Department of Science and Technology, Government of India; IITB alumni; Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) - MEXT of Japan; OISTER program
项目资助者	Research Council of Finland[324504, 328898, 353019, 340613, 350458] ; Royal Society - Science Foundation Ireland University Research Fellowship ; Eric and Wendy Schmidt A.I. in Science Fellowship ; JSPS KAKENHI[JP20H04737] ; JSPS Open Partnership Bilateral Joint Research Project between Japan and Finland - Independent Research Fund Denmark (IRFD)[JPJSBP120229923] ; Secretary of Universities and Research (Government of Catalonia) ; Horizon 2020 Research and Innovation Programme of the European Union under the Marie Sklodowska-Curie ; Beatriu de Pinos[2021 BP 00168] ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI)[PID2020-115253GA-I00] ; HOSTFLOWS project ; Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; National Natural Science Foundation of China (NSFC)[12303054] ; Yunnan Fundamental Research Projects[202401AU070063] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; UK Research and Innovation Fellowship[MR/T020784/1] ; PRIN-INAF ; MIUR, PRIN[20179ZF5KS] ; INAF GRAWITA Large Program Grant ; ESA Gaia, DPAC ; Photometric Science Alerts Team ; East Asian Observatory ; Finland and Norway ; University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias ; Instituto de Astrofisica de Andalucia (IAA) ; University of Copenhagen and NOT ; OPTICON[22A/012] ; European Union[101004719] ; Indian Institute of Astrophysics (IIA) ; Indian Institute of Technology Bombay (IITB) ; Indo-US Science and Technology Forum ; Science and Engineering Research Board, Department of Science and Technology, Government of India ; IITB alumni ; Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) - MEXT of Japan ; OISTER program
语种	英语
学科领域	天文学 ; 恒星与银河系
文章类型	Article
出版者	EDP SCIENCES S A
出版地	17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
ISSN	0004-6361
URL	查看原文
WOS记录号	WOS:001322521400028
WOS研究方向	Astronomy & Astrophysics
WOS类目	Astronomy & Astrophysics
关键词[WOS]	CORE-COLLAPSE SUPERNOVAE ; GAMMA-RAY BURST ; LIGHT CURVES ; IC SUPERNOVA ; CIRCUMSTELLAR INTERACTION ; SUPERLUMINOUS SUPERNOVAE ; OPTICAL-SPECTRA ; STAR-FORMATION ; MASSIVE STARS ; HE-STAR
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	被引频次：1[WOS] [WOS记录] [WOS相关记录]
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 & 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 & ASTROPHYSICS,689.
MLA	Kangas, T.,et al."The enigmatic double-peaked stripped-envelope SN 2023aew".ASTRONOMY & ASTROPHYSICS 689(2024).

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