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Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features

文献类型：期刊论文

作者Cai YZ(蔡永志)6,7,8; Pastorello, A.8; Maeda, K.9; Zhao, J.-W.10,11; Wang, Z.-Y.12,13; Peng, Z.-H.14; Reguitti, A.8,15; Tartaglia, L.16; Filippenko, A. V.17; Pan, Y.10,11
刊名ASTRONOMY & ASTROPHYSICS
出版日期2026-03-03
卷号707
关键词circumstellar matter supernovae: general supernovae: individual: SN 2024acyl
ISSN号0004-6361
DOI10.1051/0004-6361/202558014
产权排序第1完成单位
文献子类Article
英文摘要We present a photometric and spectroscopic analyses of the Type Ibn supernova (SN) 2024acyl. It rises to an absolute magnitude peak of M-o = -17.58 +/- 0.15 mag in 10.6 days, and displays a rapid linear post-peak light-curve decline in all bands (e.g. gamma(0 - 60)(V) = 0.097 +/- 0.002 mag day(-1)), similar to most SNe Ibn. The optical pseudobolometric light curve peaks at (3.5 +/- 0.8)& times;10(42) erg s(-1), with a total radiated energy of (5.0 +/- 0.4)& times;10(48) erg. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni He I lines and flash-ionisation emission lines of C III, N III, and He II. The P-Cygni He I features gradually evolve and become emission-dominated in late-time spectra. The H alpha line is detected throughout the entire spectral evolution, which indicates that the circumstellar material (CSM) is helium-rich with some residual amount of hydrogen. Our multi-band light-curve modelling yields estimates of the ejecta mass of M-ej = 0.49(-0.09)(+0.11) M-circle dot with a kinetic energy of E-k = 0.06(-0.01)(+0.01) & times; 10(51) erg, and a Ni-56 mass of M-Ni = 0.018 M-circle dot. The inferred CSM properties are characterised by a mass of M-CSM = 0.51(-0.04)(+0.05) M-circle dot, an inner radius of R-0=17.8(-3.0)(+3.6) AU, and a density of rho(CSM) = (8.3(-1.2)(+2.7)) & times; 10(-12) g cn(-3). The multi-epoch spectra are well reproduced by the CMFGEN/ he4p0 model, corresponding to a He-ZAMS mass of 4 M-circle dot (H-ZAMS mass 18.11 M-circle dot, pre-SN mass 3.16 M-circle dot). These findings are consistent with a scenario of an SN powered by ejecta-CSM interaction originating from a low-mass helium star that evolved within an interacting binary system where the CSM with some residual hydrogen may originate from the mass-transfer process. We also discuss an extreme scenario involving the possible merger of a helium white dwarf. In addition, a channel of core-collapse explosion of a late-type Wolf-Rayet (WR) star with hydrogen, or a transitional star between an Of and a WR type (e.g. an Ofpe/WN9 star) with fallback accretion cannot be entirely ruled out.
学科主题天文学 ; 恒星与银河系
URL标识查看原文
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
WOS关键词LIGHT-CURVE ; EMISSION-LINES ; CORE-COLLAPSE ; PROGENITOR ; EVOLUTION ; IIN ; SPECTROSCOPY ; EXPLOSION ; 2006JC ; I.
资助项目National Key Research and Development Program of China[2024YFA1611603]; National Key Research and Development Program of China[2021YFA1600404]; National Natural Science Foundation of China[12303054]; National Natural Science Foundation of China[12225304]; National Natural Science Foundation of China[12288102]; National Natural Science Foundation of China[12373038]; National Natural Science Foundation of China[12173082]; National Natural Science Foundation of China[12333008]; Yunnan Fundamental Research Projects[202401AU070063]; Yunnan Fundamental Research Projects[202501AS070078]; Yunnan Revitalization Talent Support Program (Yunling Scholar Project and Innovation Team Project); Yunnan Science and Technology Program[202501AS070005]; Yunnan Science and Technology Program[202201BC070003]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; Natural Science Foundation of Xinjiang Uygur Autonomous Region[2024D01D32]; Tianshan Talent Training Program[2023TSYCLJ0053]; PRIN-INAF 2022, Shedding light on the nature of gap transients: from the observations to the models; GRAWITA Large Program Grant; MIUR, PRIN 2020[2020KB33TP]; Japan Society for the Promotion of Science (JSPS) KAKENHI[JP24KK0070]; Japan Society for the Promotion of Science (JSPS) KAKENHI[JP24H01810]; JSPS bilateral program[JPJSBP120229923]; The Special Project for High-End Foreign Experts, Xingdian Funding from Yunnan Province; Yushan Fellow Program by the Ministry of Education, Taiwan[MOE-111-YSFMS-0008-001-P1]; National Science and Technology Council, Taiwan (NSTC)[114-2112-M-008-021-MY3]; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI)[CEX2020-001058-M]; Secretary of Universities and Research (Government of Catalonia); Horizon 2020 Research and Innovation Programme of the European Union; Marie Sklodowska-Curie; Beatriu de Pinos 2021 BP 00168 programme; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI)[PID2023-151307NB-I00]; Centro Superior de Investigaciones Cientificas (CSIC)[20215AT016]; Programme Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; Departament de Recerca i Universitats de la Generalitat de Catalunya[2021-SGR-01270]; Research Council of Finland[360274]; Research Council of Finland[350458]; Research Council of Finland[324504]; Research Council of Finland[328898]; Research Council of Finland[353019]; Leverhulme Trust[RPG-2023-240]; Independent Research Fund Denmark (IRFD); Horizon Europe ERC[101125877]; Slovenian Research Agency[I0-0033]; Slovenian Research Agency[P1-0031]; Slovenian Research Agency[J1-2460]; Slovenian Research Agency[N1-0344]; European Union - NextGenerationEU; INAF 2023 Theory Grant ObFu[1.05.23.06.06]; National Key R&D Program of China[2021YFA1600404]; Yunnan Fundamental Research Projects[202401BC070007]; Yunnan Fundamental Research Projects[202201AT070069]; Top-notch Young Talents Program of Yunnan Province; Light of West China Program provided by the Chinese Academy of Sciences; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; National Natural Science Foundation of China[12288102]; National Natural Science Foundation of China[12033003]; National Natural Science Foundation of China[11633002]; Tencent Xplorer Prize; Christopher R. Redlich Fund; CAS and the People's Government of Yunnan Province; University of Turku; Aarhus University; University of Oslo Denmark; University of Oslo Finland; University of Oslo Norway; University of Iceland; Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain of the Instituto de Astrofisica de Canarias; Instrument Centre for Danish Astrophysics (IDA); Finnish Centre for Astronomy; ESO (FINCA) via Academy of Finland[306531]; UK Science and Technology Facilities Council; The Yunnan University Development Plan for World-Class University; The Yunnan University Development Plan for World-Class Astronomy Discipline; The Key Laboratory of Survey Science of Yunnan Province[202449CE340002]; Asteroid Terrestrial-impact Last Alert System (ATLAS); National Aeronautics and Space Administration (NASA)[NN12AR55G]; National Aeronautics and Space Administration (NASA)[80NSSC18K0284]; National Aeronautics and Space Administration (NASA)[80NSSC18K1575]; Kepler/K2[J1944/80NSSC19K0112]; Kepler/K2[HST GO-15889]; STFC[ST/T000198/1]; STFC[ST/S006109/1]; NASA SSO Near Earth Observation Program[80NSSC18K0971]; NASA SSO Near Earth Observation Program[NNX14AM74G]; NASA SSO Near Earth Observation Program[NNX12AR65G]; NASA SSO Near Earth Observation Program[NNX13AQ47G]; NASA SSO Near Earth Observation Program[NNX08AR22G]; NASA SSO Near Earth Observation Program[80NSSC21K1572]; State of Hawaii; National Central University of Taiwan, STScI, NASA[NNX08AR22G]; Planetary Science Division of the NASA Science Mission Directorate, NSF[AST-1238877]; University of Maryland, Eotvos Lorand University (ELTE); Los Alamos National Laboratory; Gordon and Betty Moore Foundation
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001705367900001
出版者EDP SCIENCES S A
资助机构National Key Research and Development Program of China[2024YFA1611603, 2021YFA1600404] ; National Natural Science Foundation of China[12303054, 12225304, 12288102, 12373038, 12173082, 12333008] ; Yunnan Fundamental Research Projects[202401AU070063, 202501AS070078] ; Yunnan Revitalization Talent Support Program (Yunling Scholar Project and Innovation Team Project) ; Yunnan Science and Technology Program[202501AS070005, 202201BC070003] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; Natural Science Foundation of Xinjiang Uygur Autonomous Region[2024D01D32] ; Tianshan Talent Training Program[2023TSYCLJ0053] ; PRIN-INAF 2022, Shedding light on the nature of gap transients: from the observations to the models ; GRAWITA Large Program Grant ; MIUR, PRIN 2020[2020KB33TP] ; Japan Society for the Promotion of Science (JSPS) KAKENHI[JP24KK0070, JP24H01810] ; JSPS bilateral program[JPJSBP120229923] ; The Special Project for High-End Foreign Experts, Xingdian Funding from Yunnan Province ; Yushan Fellow Program by the Ministry of Education, Taiwan[MOE-111-YSFMS-0008-001-P1] ; National Science and Technology Council, Taiwan (NSTC)[114-2112-M-008-021-MY3] ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI)[CEX2020-001058-M] ; Secretary of Universities and Research (Government of Catalonia) ; Horizon 2020 Research and Innovation Programme of the European Union ; Marie Sklodowska-Curie ; Beatriu de Pinos 2021 BP 00168 programme ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI)[PID2023-151307NB-I00] ; Centro Superior de Investigaciones Cientificas (CSIC)[20215AT016] ; Programme Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; Departament de Recerca i Universitats de la Generalitat de Catalunya[2021-SGR-01270] ; Research Council of Finland[360274, 350458, 324504, 328898, 353019] ; Leverhulme Trust[RPG-2023-240] ; Independent Research Fund Denmark (IRFD) ; Horizon Europe ERC[101125877] ; Slovenian Research Agency[I0-0033, P1-0031, J1-2460, N1-0344] ; European Union - NextGenerationEU ; INAF 2023 Theory Grant ObFu[1.05.23.06.06] ; National Key R&D Program of China[2021YFA1600404] ; Yunnan Fundamental Research Projects[202401BC070007, 202201AT070069] ; Top-notch Young Talents Program of Yunnan Province ; Light of West China Program provided by the Chinese Academy of Sciences ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; National Natural Science Foundation of China[12288102, 12033003, 11633002] ; Tencent Xplorer Prize ; Christopher R. Redlich Fund ; CAS and the People's Government of Yunnan Province ; University of Turku ; Aarhus University ; University of Oslo Denmark ; University of Oslo Finland ; University of Oslo Norway ; University of Iceland ; Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain of the Instituto de Astrofisica de Canarias ; Instrument Centre for Danish Astrophysics (IDA) ; Finnish Centre for Astronomy ; ESO (FINCA) via Academy of Finland[306531] ; UK Science and Technology Facilities Council ; The Yunnan University Development Plan for World-Class University ; The Yunnan University Development Plan for World-Class Astronomy Discipline ; The Key Laboratory of Survey Science of Yunnan Province[202449CE340002] ; Asteroid Terrestrial-impact Last Alert System (ATLAS) ; National Aeronautics and Space Administration (NASA)[NN12AR55G, 80NSSC18K0284, 80NSSC18K1575] ; Kepler/K2[J1944/80NSSC19K0112, HST GO-15889] ; STFC[ST/T000198/1, ST/S006109/1] ; NASA SSO Near Earth Observation Program[80NSSC18K0971, NNX14AM74G, NNX12AR65G, NNX13AQ47G, NNX08AR22G, 80NSSC21K1572] ; State of Hawaii ; National Central University of Taiwan, STScI, NASA[NNX08AR22G] ; Planetary Science Division of the NASA Science Mission Directorate, NSF[AST-1238877] ; University of Maryland, Eotvos Lorand University (ELTE) ; Los Alamos National Laboratory ; Gordon and Betty Moore Foundation
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/29022]  
专题云南天文台_大样本恒星演化研究组
通讯作者Cai YZ(蔡永志); Wang B(王博); Wang, X.-F.
作者单位1.Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast Belfast BT7 1NN, UK;
2.Department of Physics, Tsinghua University Beijing 100084, P.R. China;
3.National Astronomical Observatory of Japan, National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo 181-8588, Japan;
4.Dipartimento di Fisica “Ettore Pancini”, Università di Napoli Federico II Via Cinthia 9 80126 Naples, Italy;
5.Purple Mountain Observatory, Chinese Academy of Sciences Nanjing 210023, P.R. China
6.Yunnan Observatories, Chinese Academy of Sciences Kunming 650216, P.R. China;
7.International Centre of Supernovae, Yunnan Key Laboratory Kunming 650216, P.R. China;
8.INAF – Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 35122 Padova, Italy;
9.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku Kyoto 606-8502, Japan;
10.South-Western Institute for Astronomy Research, Yunnan University Kunming 650500, P.R. China;
推荐引用方式
GB/T 7714		 Cai YZ,Pastorello, A.,Maeda, K.,et al. Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features[J]. ASTRONOMY & ASTROPHYSICS,2026,707.
APA 蔡永志.,Pastorello, A..,Maeda, K..,Zhao, J.-W..,Wang, Z.-Y..,...&Wang, X.-F..(2026).Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features.ASTRONOMY & ASTROPHYSICS,707.
MLA 蔡永志,et al."Massive stars exploding in a He-rich circumstellar medium XII. SN 2024acyl: A fast, linearly declining Type Ibn supernova with early flash-ionisation features".ASTRONOMY & ASTROPHYSICS 707(2026).

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