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The diversity of strongly interacting Type IIn supernovae

文献类型：期刊论文

作者Salmaso, I.18; Cappellaro, E.18; Tartaglia, L.18,19; Anderson, J. P.20,21; Benetti, S.18; Bronikowski, M.22; Cai YZ(蔡永志)17,23,24; Charalampopoulos, P.15; Chen, T.-W.14; Concepcion, E.22
刊名ASTRONOMY & ASTROPHYSICS
出版日期2025-02-27
卷号695
关键词neutrinos supernovae: general supernovae: individual: 2021acya supernovae: individual: 2021adxl supernovae: individual: 2022qml supernovae: individual: 2022wed
ISSN号0004-6361
DOI10.1051/0004-6361/202451764
产权排序第6完成单位
文献子类Article
英文摘要Context. At late stages, massive stars experience strong mass-loss rates, losing their external layers and thus producing a dense H-rich circumstellar medium (CSM). After the explosion of a massive star, the collision and continued interaction of the supernova (SN) ejecta with the CSM power the SN light curve through the conversion of kinetic energy into radiation. When the interaction is strong, the light curve shows a broad peak and high luminosity that lasts for several months. For these SNe, the spectral evolution is also slower compared to non-interacting SNe. Notably, energetic shocks between the ejecta and the CSM create the ideal conditions for particle acceleration and the production of high-energy (HE) neutrinos above 1 TeV. Aims. We study four strongly interacting Type IIn SNe, 2021acya, 2021adxl, 2022qml, and 2022wed, in order to highlight their peculiar characteristics, derive the kinetic energy of their explosion and the characteristics of the CSM, infer clues on the possible progenitors and their environment, and relate them to the production of HE neutrinos. Methods. We analysed spectro-photometric data of a sample of interacting SNe to determine their common characteristics and derive the physical properties (radii and masses) of the CSM and the ejecta kinetic energies and compare them to HE neutrino production models. Results. The SNe analysed in this sample exploded in dwarf star-forming galaxies, and they are consistent with energetic explosions and strong interaction with the surrounding CSM. For SNe 2021acya and 2022wed, we find high CSM masses and mass-loss rates, linking them to very massive progenitors. For SN 2021adxl, the spectral analysis and less extreme CSM mass suggest a stripped-envelope massive star as a possible progenitor. SN 2022qml is marginally consistent with being a Type Ia thermonuclear explosion embedded in a dense CSM. The mass-loss rates for all the SNe are consistent with the expulsion of several solar masses of material during eruptive episodes in the last few decades before the explosion. Finally, we find that the SNe in our sample are marginally consistent with HE neutrino production.
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GAMMA-RAY BURST ; CIRCUMSTELLAR INTERACTION ; SUPERLUMINOUS SUPERNOVAE ; SN 2010JL ; PRESUPERNOVA EVOLUTION ; STELLAR MASS ; LIGHT CURVES ; EMISSION ; DUST ; SPECTRA
资助项目MIUR[20179ZF5KS]; PRIN-INAF 2022 project Shedding light on the nature of gap transients: from the observations to the models; National Natural Science Foundation of China (NSFC)[12303054]; National Key Research and Development Program of China[2024YFA1611603]; Yunnan Fundamental Research Projects[202401AU070063]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; Millennium Science Initiative[ICN12_009]; ANID through the Beca Doctorado Nacional[202221222222]; European Research Council (ERC) under the European Union[948381]; UK Space Agency[ST/Y000692/1]; Spanish Ministerio de Ciencia e Innovacin (MCIN); Agencia Estatal de Investigacin (AEI); European Social Fund (ESF) Investing in your future; European Union Next Generation EU/PRTR funds; Horizon 2020 Research and Innovation Programme of the European Union; Secretary of Universities and Research (Government of Catalonia)[PID2020-115253GA-I00 HOSTFLOWS]; Secretary of Universities and Research (Government of Catalonia)[2021-SGR-01270]; Secretary of Universities and Research (Government of Catalonia)[RYC2019-027683-I]; Secretary of Universities and Research (Government of Catalonia)[FJC2021-047124-I]; Secretary of Universities and Research (Government of Catalonia)[2021 BP 00168]; Centro Superior de Investigaciones Cientficas (CSIC) under the PIE project[20215AT016]; Program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; Ministry of Education, Taiwan; EC; Slovenian Research Agency[I0-0033]; Slovenian Research Agency[P1-0031]; Slovenian Research Agency[J1-8136]; Slovenian Research Agency[J1-2460]; Slovenian Research Agency[Z1-1853]; Research Council of Finland[340613]; Independent Research Fund Denmark[10.46540/2032-00022B]; European Union; University of Turku; Aarhus University; University of Iceland; Instrument Centre for Danish Astrophysics (IDA); Instituto de Astrofisica de Andalucia (IAA); NSF[AST-1911225]; NSF[AST-1911151]; NASA SWIFT grant[80NSSC19K1639]; UK Science and Technology Facilities Council; INAF; Spanish Government; Canary Islands through the European Funds for Regional Development (FEDER); US University of Florida; European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes[1103.D-0328]; European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes[105.20TF.001]; National Science Foundation[AST-1238877]; Weizmann Institute for Science; Oskar Klein Center at Stockholm University; University of Maryland, Deutsches Elektronen-Synchrotron; TANGO Consortium of Taiwan; Lawrence Livermore National Laboratories; IN2P3, France; Max-Planck Society; Max Planck Institute for Extraterrestrial Physics; Queen's University Belfast; National Central University of Taiwan; Space Telescope Science Institute; National Aeronautics and Space Administration[NNX08AR22G]; NASA Science Mission Directorate; University of Maryland, Eotvos Lorand University (ELTE); Los Alamos National Laboratory; Gordon and Betty Moore Foundation; Asteroid Terrestrial-impact Last Alert System (ATLAS) project; Asteroid Terrestrial-impact Last Alert System (ATLAS); NASA[NN12AR55G]; NASA[80NSSC18K0284]; NASA[80NSSC18K1575]; NASA[J1944/80NSSC19K0112]; NASA[HST GO-15889]; STFC[ST/T000198/1]; STFC[ST/S006109/1]; South African Astronomical Observatory
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001434064300011
出版者EDP SCIENCES S A
资助机构MIUR[20179ZF5KS] ; PRIN-INAF 2022 project Shedding light on the nature of gap transients: from the observations to the models ; National Natural Science Foundation of China (NSFC)[12303054] ; National Key Research and Development Program of China[2024YFA1611603] ; Yunnan Fundamental Research Projects[202401AU070063] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; Millennium Science Initiative[ICN12_009] ; ANID through the Beca Doctorado Nacional[202221222222] ; European Research Council (ERC) under the European Union[948381] ; UK Space Agency[ST/Y000692/1] ; Spanish Ministerio de Ciencia e Innovacin (MCIN) ; Agencia Estatal de Investigacin (AEI) ; European Social Fund (ESF) Investing in your future ; European Union Next Generation EU/PRTR funds ; Horizon 2020 Research and Innovation Programme of the European Union ; Secretary of Universities and Research (Government of Catalonia)[PID2020-115253GA-I00 HOSTFLOWS, 2021-SGR-01270, RYC2019-027683-I, FJC2021-047124-I, 2021 BP 00168] ; Centro Superior de Investigaciones Cientficas (CSIC) under the PIE project[20215AT016] ; Program Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; Ministry of Education, Taiwan ; EC ; Slovenian Research Agency[I0-0033, P1-0031, J1-8136, J1-2460, Z1-1853] ; Research Council of Finland[340613] ; Independent Research Fund Denmark[10.46540/2032-00022B] ; European Union ; University of Turku ; Aarhus University ; University of Iceland ; Instrument Centre for Danish Astrophysics (IDA) ; Instituto de Astrofisica de Andalucia (IAA) ; NSF[AST-1911225, AST-1911151] ; NASA SWIFT grant[80NSSC19K1639] ; UK Science and Technology Facilities Council ; INAF ; Spanish Government ; Canary Islands through the European Funds for Regional Development (FEDER) ; US University of Florida ; European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes[1103.D-0328, 105.20TF.001] ; National Science Foundation[AST-1238877] ; Weizmann Institute for Science ; Oskar Klein Center at Stockholm University ; University of Maryland, Deutsches Elektronen-Synchrotron ; TANGO Consortium of Taiwan ; Lawrence Livermore National Laboratories ; IN2P3, France ; Max-Planck Society ; Max Planck Institute for Extraterrestrial Physics ; Queen's University Belfast ; National Central University of Taiwan ; Space Telescope Science Institute ; National Aeronautics and Space Administration[NNX08AR22G] ; NASA Science Mission Directorate ; University of Maryland, Eotvos Lorand University (ELTE) ; Los Alamos National Laboratory ; Gordon and Betty Moore Foundation ; Asteroid Terrestrial-impact Last Alert System (ATLAS) project ; Asteroid Terrestrial-impact Last Alert System (ATLAS) ; NASA[NN12AR55G, 80NSSC18K0284, 80NSSC18K1575, J1944/80NSSC19K0112, HST GO-15889] ; STFC[ST/T000198/1, ST/S006109/1] ; South African Astronomical Observatory
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/28181]  
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.Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warszawa, Poland;
2.The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 106 91 Stockholm, Sweden;
3.Nordic Optical Telescope, Aarhus Universitet, Rambla José Ana Fernández Pérez 7, local 5, E-38711 San Antonio, Breña Baja Santa Cruz de Tenerife, Spain;
4.Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Vesilinnantie 5, 20014 Turku, Finland;
5.Astrophysics Research Institute, Liverpool John Moores University, ic2, 146 Brownlow Hill, Liverpool L3 5RF, UK;
6.Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, Germany;
7.Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK;
8.Instituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile;
9.Instituto de Alta Investigación, Universidad de Tarapacá, Casilla 7D, Arica, Chile;
10.INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, (LC), Italy;
推荐引用方式
GB/T 7714		 Salmaso, I.,Cappellaro, E.,Tartaglia, L.,et al. The diversity of strongly interacting Type IIn supernovae[J]. ASTRONOMY & ASTROPHYSICS,2025,695.
APA Salmaso, I..,Cappellaro, E..,Tartaglia, L..,Anderson, J. P..,Benetti, S..,...&Valerin, G..(2025).The diversity of strongly interacting Type IIn supernovae.ASTRONOMY & ASTROPHYSICS,695.
MLA Salmaso, I.,et al."The diversity of strongly interacting Type IIn supernovae".ASTRONOMY & ASTROPHYSICS 695(2025).

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