2020/04/12 by Jie Lin, Rui-Jing Lu, Da-Bin Lin +1 · 10 citations
Physics and Astronomy · #Accretion (finance) #Afterglow #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Ejecta #Galaxy #Gamma-ray burst #Gamma-ray bursts and supernovae #Light curve #Magnetar #Neutron star #Physics #Pulsars and Gravitational Waves Research #Redshift #Supernova #astro-ph.HE
paper · pdf · doi:10.3847/1538-4357/ab88a7
published in The Astrophysical Journal 895(1), 46 (IOP Publishing) · 15 pages, 3 figures. To be accepted for publication in ApJ
arxiv created 2020/04/12 · openalex publication_date 2020/05/01 · arxiv updated 2020/06/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Ultra-long-duration gamma-ray burst GRB 111209A was found to be associated with a very luminous supernovae (SNe) SN 2011kl. The physics of GRB 111209A/SN 2011kl has been extensively studied in the literature, but such research has not yet settled down. By investigating in detail the characteristics of the X-ray light curve of GRB 111209A, coupled with the temporal and spectral features observed in SN 2011kl, we argue that a short-lived supramassive magnetar could be responsible for the initial shallow X-ray emission. Then the electromagnetic extraction of spin energy from a black hole (BH) results in the steeply declining X-ray flux when the magnetar collapses into a BH. A fraction of the envelope materials falls back and activates the accretion onto the newborn BH, which produces the X-ray rebrightening bump at late times. During this process, a centrifugally driven baryon-rich quasi-isotropic Blandford & Payne outflow from the revived accretion disk deposits its kinetic energy on the SN ejecta, which powers luminous SN 2011kl. Finally, we place a limitation on the magnetar’s physical parameters based on the observations.