| The metamorphosis of the Type Ib SN 2019yvr: late-time interaction | |
Ferrari, Lucía1,2; Folatelli, Gastón1,2,3; Kuncarayakti, Hanindyo4,5; Stritzinger, Maximilian6; Maeda, Keiichi7; Bersten, Melina1,2,3; Aguilar, Lili M Román1,2; Sáez, M Manuela8,9; Dessart, Luc10; Lundqvist, Peter11; Mazzali, Paolo12,13; Nagao, Takashi4,14,15; Ashall, Chris16; Bose, Subhash6,17; Brennan, Seán J11; Cai YZ(蔡永志)18,19,20 ; Handberg, Rasmus6; Holmbo, Simon6; Karamehmetoglu, Emir6; Pastorello, Andrea21; Reguitti, Andrea21,22; Anderson, Joseph23; Chen, Ting-Wan24; Galbany, Lluís25,26; Gromadzki, Mariusz27; Gutiérrez, Claudia P25,26; Inserra, Cosimo28; Kankare, Erkki4; Bravo, Tomás E Müller25,26; Mattila, Seppo4,29; Nicholl, Matt30; Pignata, Giuliano31; Sollerman, Jesper11; Srivastav, Shubham32; Young, David R32
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| 发表期刊 | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
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| 2024-12-28 | |
| 卷号 | 529期号:1页码:L33-L40 |
| DOI | 10.1093/mnrasl/slad195 |
| 产权排序 | 第18完成单位 |
| 收录类别 | SCI |
| 关键词 | supernovae: general supernovae: individual: SN 2019yvr |
| 摘要 | We present observational evidence of late-time interaction between the ejecta of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow H alpha emission line appears simultaneously with a break in the light-curve decline rate at around 80-100d after explosion. From the interaction delay and the ejecta velocity, under the assumption that the CSM is detached from the progenitor, we estimate the CSM inner radius to be located at similar to 6.5-9.1 x 10(15) cm. The H alpha emission line persists throughout the nebular phase at least up to +420d post-explosion, with a full width at half maximum of similar to 2000 km s(-1). Assuming a steady mass-loss, the estimated mass-loss rate from the luminosity of the H alpha line is similar to 3-7 x 10(-5) M-circle dot yr(-1). From hydrodynamical modelling and analysis of the nebular spectra, we find a progenitor He-core mass of 3-4 M-circle dot, which would imply an initial mass of 13-15 M-circle dot. Our result supports the case of a relatively low-mass progenitor possibly in a binary system as opposed to a higher mass single star undergoing a luminous blue variable phase. |
| 资助项目 | Finnish National Agency for Education (EDUFI); Research Council of Finland[324504]; Research Council of Finland[328898]; Research Council of Finland[353019]; Research Council of Finland[350458]; Independent Research Fund Denmark (IRFD); Japan Society for the Promotion of Science (JSPS) KAKENHI[JP20H00174]; JSPS[JPJSBP120229923]; NUTS; OPTICON[2020A/031]; NOAO[NOAO2020A-017]; National Natural Science Foundation of China (NSFC)[12303054]; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001]; PRIN-INAF; Spanish Ministerio de Ciencia e Innovacion (MCIN); Agencia Estatal de Investigacion (AEI); European Social Fund (ESF)[RYC2019-027683-I]; HOSTFLOWS project[PID2020-115253GA-I00]; Centro Superior de Investigaciones Cientificas (CSIC)[20215AT016]; programme Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M]; Secretary of Universities and Research (Government of Catalonia); European Union under the Marie SklodowskaCurie; Beatriu de Pinos 2021 BP 00168 programme; Agencia Estatal de Investigacion (AEI)[PID2020-115253GA-I00]; European Union Next Generation EU/PRTR funds[FJC2021-047124-I]; Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project[20215AT016]; European Research Council (ERC) under the European Union[948381]; UK Space Agency[ST/Y000692/1]; ANID through Millennium Science Initiative Programs |
| 项目资助者 | Finnish National Agency for Education (EDUFI) ; Research Council of Finland[324504, 328898, 353019, 350458] ; Independent Research Fund Denmark (IRFD) ; Japan Society for the Promotion of Science (JSPS) KAKENHI[JP20H00174] ; JSPS[JPJSBP120229923] ; NUTS ; OPTICON[2020A/031] ; NOAO[NOAO2020A-017] ; National Natural Science Foundation of China (NSFC)[12303054] ; International Centre of Supernovae, Yunnan Key Laboratory[202302AN360001] ; PRIN-INAF ; Spanish Ministerio de Ciencia e Innovacion (MCIN) ; Agencia Estatal de Investigacion (AEI) ; European Social Fund (ESF)[RYC2019-027683-I] ; HOSTFLOWS project[PID2020-115253GA-I00] ; Centro Superior de Investigaciones Cientificas (CSIC)[20215AT016] ; programme Unidad de Excelencia Maria de Maeztu[CEX2020-001058-M] ; Secretary of Universities and Research (Government of Catalonia) ; European Union under the Marie SklodowskaCurie ; Beatriu de Pinos 2021 BP 00168 programme ; Agencia Estatal de Investigacion (AEI)[PID2020-115253GA-I00] ; European Union Next Generation EU/PRTR funds[FJC2021-047124-I] ; Centro Superior de Investigaciones Cientificas (CSIC) under the PIE project[20215AT016] ; European Research Council (ERC) under the European Union[948381] ; UK Space Agency[ST/Y000692/1] ; ANID through Millennium Science Initiative Programs[ICN12 009] ; [PID2020-115253GAI00] |
| 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 | OXFORD UNIV PRESS |
| 出版地 | GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND |
| ISSN | 0035-8711 |
| URL | 查看原文 |
| WOS记录号 | WOS:001305964600001 |
| WOS研究方向 | Astronomy & Astrophysics |
| WOS类目 | Astronomy & Astrophysics |
| 关键词[WOS] | CORE-COLLAPSE ; MASSIVE STARS ; CIRCUMSTELLAR INTERACTION ; NEBULAR SPECTRA ; LATE EMISSION ; SUPERNOVA ; ENVELOPE ; EVOLUTION ; NUCLEOSYNTHESIS ; PROGENITOR |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 版本 | 出版稿 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/27589 |
| 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.Instituto de Astrofísica de La Plata, CONICET, B1900FWA, La Plata, Argentina; 2.Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata, Paseo del Bosque S/N B1900FWA, La Plata, Argentina; 3.Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, 277-8583 Chiba, Japan; 4.Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland; 5.Finnish Centre for Astronomy with ESO (FINCA), University of Turku, FI-20014, Finland; 6.Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark; 7.Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan; 8.Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako, Saitama 351-0198, Japan; 9.Department of Physics, University of California, Berkeley, CA 94720, United States of America; 10.Institut d’Astrophysique de Paris, CNRS-Sorbonne Université, 98 bis boulevard Arago, F-75014 Paris, France; 11.The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, SE-10691 Stockholm, Sweden; 12.Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany; 13.Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UK; 14.Metsähovi Radio Observatory, Aalto University, Metsähovintie 114, FI-02540 Kylmälä, Finland; 15.Department of Electronics and Nanoengineering, Aalto University, P.O. BOX 15500, FI-00076 AALTO, Finland; 16.Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA; 17.Department of Astronomy, The Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210, USA; 18.Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, P.R. China; 19.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, P.R. China; 20.International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, P.R. China; 21.INAF - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy; 22.INAF - Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate (LC), Italy; 23.European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile; 24.Graduate Institute of Astronomy, National Central University, 300 Jhongda Road, 32001 Jhongli, Taiwan; 25.Institute of Space Sciences (ICE-CSIC), Campus UAB, Carrer de Can Magrans, s/n, E-08193 Barcelona, Spain; 26.Institut d’Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain; 27.Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, PL-00-478 Warszawa, Poland; 28.School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK; 29.School of Sciences, European University Cyprus, Diogenes Street, Engomi, 1516, Nicosia, Cyprus; 30.Astrophysics Research Centre, School of Mathematics and Physics, Queens University Belfast, Belfast BT7 1NN, UK; 31.Instituto de Alta Investigación, Universidad de Tarapacá, Casilla 7D, 1001236, Arica, Chile; 32.Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK |
| 推荐引用方式 GB/T 7714 | Ferrari, Lucía,Folatelli, Gastón,Kuncarayakti, Hanindyo,et al. The metamorphosis of the Type Ib SN 2019yvr: late-time interaction[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2024,529(1):L33-L40. |
| APA | Ferrari, Lucía.,Folatelli, Gastón.,Kuncarayakti, Hanindyo.,Stritzinger, Maximilian.,Maeda, Keiichi.,...&Young, David R.(2024).The metamorphosis of the Type Ib SN 2019yvr: late-time interaction.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,529(1),L33-L40. |
| MLA | Ferrari, Lucía,et al."The metamorphosis of the Type Ib SN 2019yvr: late-time interaction".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 529.1(2024):L33-L40. |
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