Hidden shock powering the peak of SN 2020faa
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Archivos
Fecha
2023
Profesor/a Guía
Facultad/escuela
Idioma
en
Título de la revista
ISSN de la revista
Título del volumen
Editor
EDP Sciences
Nombre de Curso
Licencia CC
CC BY 4.0 Attribution 4.0 International Deed
Licencia CC
https://creativecommons.org/licenses/by/4.0/
Resumen
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 Mo, and kinetic energy, Ekin(shell) = 0.9-0.3+0.5 × 1051 erg, and a core with Mcore = 21.5-0.7+1.4 Mo 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. © The Authors 2023.
Notas
Indexación: Scopus
Palabras clave
Stars: Massive, Supernovae: General, Supernovae: individual: SN 2020faa
Citación
Astronomy and Astrophysics. Volume 6731. May 2023. Article number A127
DOI
10.1051/0004-6361/202245781