Abstract
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.
Highlights
Gamma-Ray Bursts (GRBs) are the most luminous explosions in the universe since the big bang, and are commonly divided into short GRBs and long GRBs (LGRBs), with a separation around T90 ≈ 2s
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-living supramassive magnetar can be responsible for the initial shallow X-ray emission
If ultra-long GRBs (ULGRBs) originates from the core collapse of massive stars, its central engine falls into two classes: a hyperaccreting stellar-mass black hole (BH) (Woosley 1993) or a neutron stars (NSs) with millisecond rotation period and an ultrastrong magnetic field (Usov 1992; Dai & Liu 2012; Zhang & Meszaros 2001; Cano et al 2017; Gompertz, & Fruchter 2017)
Summary
Gamma-Ray Bursts (GRBs) are the most luminous explosions in the universe since the big bang, and are commonly divided into short GRBs and long GRBs (LGRBs), with a separation around T90 ≈ 2s (where T90 is the time window containing 90% of the energy released, Kouveliotou et al 1993). By comprehensive analyses of the data from the X-shooter instrument on the Very Large Telescope (Vernet et al 2011) near the peak of the excess emission (29 December 2011), Greiner et al (2015) found that SN 2011kl is spectroscopically associated with ultra-long GRB 111209A Their further investigations showed that this supernova with a peak luminostiy ∼ 3.63 × 1043 erg s−1 is more than three times more luminous than type Ic SNe. The time of peak brightness of SN 2011kl is ∼ 14 days, slightly larger than the average (13.0 days with a standard deviation of 2.7 days; Cano et al 2017) of other GRB-SNe. At the same time, its spectrum appears rather featureless, resembling those of super-luminous SNe, but extends further down into the rest-frame ultraviolet. Kann et al (2019) performed the supernova fitting together with considering a filter-dependent host-galaxy component at very late times, and derived the bolometric light curve of SN 2011kl, as shown in Fig. (2)
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