Close, bright, and boxy: the superluminous SN 2018hti
No hay miniatura disponible
Archivos
Fecha
2022-05-01
Profesor/a Guía
Facultad/escuela
Idioma
en
Título de la revista
ISSN de la revista
Título del volumen
Editor
Oxford University Press
Nombre de Curso
Licencia CC
https://creativecommons.org/licenses/by/4.0/deed.es
Licencia CC
CC BY 4.0 DEED
Atribución 4.0 Internacional
Resumen
SN 2018hti was a very nearby (z = 0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -21.7 mag in r band at maximum. The densely sampled pre-maximum light curves of SN 2018hti show a slow luminosity evolution and constrain the rise time to ∼50 rest-frame d. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ∼10 M⊙ of circumstellar material or a magnetar with a magnetic field of Bp∼1.3 × 1013 G, and initial period of Pspin∼1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ∼40M⊙ progenitor star. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
Notas
Indexación: Scopus.
Palabras clave
Supernovae: general, Supernovae: individual: SN 2018hti, Supernovae, Circumstellar materials, Light curves, Magnetars, Magnetic-field, Physical parameters, Risetimes, Spectra modeling, Supernovae: individual: sn 1987a
Citación
Monthly Notices of the Royal Astronomical Society, Volume 512, Issue 3, Pages 4484 - 4502, 1 May 2022
DOI
10.1093/mnras/stac744