Hidden shock powering the peak of SN 2020faa

[Context] The link between the fate of the most massive stars and the resulting supernova (SN) explosion is still a matter of debate, in major part because of the ambiguity among light-curve powering mechanisms. When stars explode as SNe, the light-curve luminosity is typically sustained by a centra...

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Autores: Salmaso, Irene, Cappellaro, Enrico, Tartaglia, Leonardo, Benetti, Stefano, Botticella, M.T., Elias-Rosa, Nancy, Pastorello, Andrea, Patat, Ferdinando, Reguitti, Andrea, Tomasella, Lina, Valerin, Giorgio, Yang, Shikuan
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/336717
Acceso en línea:http://hdl.handle.net/10261/336717
Access Level:acceso abierto
Palabra clave:Supernovae: general
Supernovae: individual: SN 2020faa
Stars: massive
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spelling Hidden shock powering the peak of SN 2020faaSalmaso, IreneCappellaro, EnricoTartaglia, LeonardoBenetti, StefanoBotticella, M.T.Elias-Rosa, NancyPastorello, AndreaPatat, FerdinandoReguitti, AndreaTomasella, LinaValerin, GiorgioYang, ShikuanSupernovae: generalSupernovae: individual: SN 2020faaStars: massive[Context] The link between the fate of the most massive stars and the resulting supernova (SN) explosion is still a matter of debate, in major part because of the ambiguity among light-curve powering mechanisms. When stars explode as SNe, the light-curve luminosity is typically sustained by a central engine (radioactive decay, magnetar spin-down, or fallback accretion). However, since massive stars eject considerable amounts of material during their evolution, there may be a significant contribution coming from interactions with the previously ejected circumstellar medium (CSM). Reconstructing the progenitor configuration at the time of explosion requires a detailed analysis of the long-term photometric and spectroscopic evolution of the related transient.[Aims] In this paper, we present the results of our follow-up campaign of SN 2020faa. Given the high luminosity and peculiar slow light curve, it is purported to have a massive progenitor. We present the spectro-photometric dataset and investigate different options to explain the unusual observed properties that support this assumption.[Methods] We computed the bolometric luminosity of the supernova and the evolution of its temperature, radius, and expansion velocity. We also fit the observed light curve with a multi-component model to infer information on the progenitor and the explosion mechanism.[Results] Reasonable parameters are inferred for SN 2020faa with a magnetar of energy, Ep = 1.5−0.2+0.5 × 1050 erg, and spin-down time, tspin = 15 ± 1 d, a shell mass, Mshell = 2.4−0.4+0.5 M⊙, and kinetic energy, Ekin(shell) = 0.9−0.3+0.5 × 1051 erg, and a core with Mcore = 21.5−0.7+1.4 M⊙ and Ekin(core) = 3.9−0.4+0.1 × 1051 erg. In addition, we need an extra source to power the luminosity of the second peak. We find that a hidden interaction with either a CSM disc or several delayed and choked jets is a viable mechanism for supplying the required energy to achieve this effect.This paper is supported by fundings from MIUR, PRIN 2017 (grant 20179ZF5KS). IS, EC, SB, MTB, NER, AP, and LT are partially supported by the PRIN-INAF 2022 project “Shedding light on the nature of gap transients: from the observations to the models”. IS acknowledges the support of the doctoral grant funded by Istituto Nazionale di Astrofisica via the University of Padova and the Italian Ministry of Education, University and Research (MIUR). AR acknowledges support from ANID BECAS/DOCTORADO NACIONAL 21202412. GV acknowledges INAF for funding his PhD fellowship within the PhD School in Astronomy at the University of Padova. The project is actively supported by the Spanish Government and the Local Government from the Canary Islands through the European Funds for Regional Development (FEDER) provided by the European Union.Peer reviewedEDP SciencesMinistero dell'Istruzione, dell'Università e della RicercaEuropean CommissionIstituto Nazionale di AstrofisicaUniversità degli Studi di PadovaGobierno de CanariasAgencia Nacional de Investigación y Desarrollo (Chile)European CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202320232023info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionapplication/pdfhttp://hdl.handle.net/10261/336717reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttps://doi.org/10.1051/0004-6361/202245781Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3367172026-05-22T06:33:51Z
dc.title.none.fl_str_mv Hidden shock powering the peak of SN 2020faa
title Hidden shock powering the peak of SN 2020faa
spellingShingle Hidden shock powering the peak of SN 2020faa
Salmaso, Irene
Supernovae: general
Supernovae: individual: SN 2020faa
Stars: massive
title_short Hidden shock powering the peak of SN 2020faa
title_full Hidden shock powering the peak of SN 2020faa
title_fullStr Hidden shock powering the peak of SN 2020faa
title_full_unstemmed Hidden shock powering the peak of SN 2020faa
title_sort Hidden shock powering the peak of SN 2020faa
dc.creator.none.fl_str_mv Salmaso, Irene
Cappellaro, Enrico
Tartaglia, Leonardo
Benetti, Stefano
Botticella, M.T.
Elias-Rosa, Nancy
Pastorello, Andrea
Patat, Ferdinando
Reguitti, Andrea
Tomasella, Lina
Valerin, Giorgio
Yang, Shikuan
author Salmaso, Irene
author_facet Salmaso, Irene
Cappellaro, Enrico
Tartaglia, Leonardo
Benetti, Stefano
Botticella, M.T.
Elias-Rosa, Nancy
Pastorello, Andrea
Patat, Ferdinando
Reguitti, Andrea
Tomasella, Lina
Valerin, Giorgio
Yang, Shikuan
author_role author
author2 Cappellaro, Enrico
Tartaglia, Leonardo
Benetti, Stefano
Botticella, M.T.
Elias-Rosa, Nancy
Pastorello, Andrea
Patat, Ferdinando
Reguitti, Andrea
Tomasella, Lina
Valerin, Giorgio
Yang, Shikuan
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministero dell'Istruzione, dell'Università e della Ricerca
European Commission
Istituto Nazionale di Astrofisica
Università degli Studi di Padova
Gobierno de Canarias
Agencia Nacional de Investigación y Desarrollo (Chile)
European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Supernovae: general
Supernovae: individual: SN 2020faa
Stars: massive
topic Supernovae: general
Supernovae: individual: SN 2020faa
Stars: massive
description [Context] The link between the fate of the most massive stars and the resulting supernova (SN) explosion is still a matter of debate, in major part because of the ambiguity among light-curve powering mechanisms. When stars explode as SNe, the light-curve luminosity is typically sustained by a central engine (radioactive decay, magnetar spin-down, or fallback accretion). However, since massive stars eject considerable amounts of material during their evolution, there may be a significant contribution coming from interactions with the previously ejected circumstellar medium (CSM). Reconstructing the progenitor configuration at the time of explosion requires a detailed analysis of the long-term photometric and spectroscopic evolution of the related transient.
publishDate 2023
dc.date.none.fl_str_mv 2023
2023
2023
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/336717
url http://hdl.handle.net/10261/336717
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv https://doi.org/10.1051/0004-6361/202245781
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,81155

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