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A GRB Afterglow Model Consistent with Hypernova Observations
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DOI：10.3847/1538-4357/aaeac8.png)
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Abstract
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We describe the afterglows of the long gamma-ray-burst (GRB) 130427A within the context of a binary-driven hypernova. The afterglows originate from the interaction between a newly born neutron star (nu NS), created by an Ic supernova (SN), and a mildly relativistic ejecta of a hypernova (HN). Such an HN in turn results from the impact of the GRB on the original SN Ic. The mildly relativistic expansion velocity of the afterglow (Gamma similar to 3) is determined, using our model-independent approach, from the thermal emission between 196 and 461 s. The power law in the optical and X-ray bands of the afterglow is shown to arise from the synchrotron emission of relativistic electrons in the expanding magnetized HN ejecta. Two components contribute to the injected energy: the kinetic energy of the mildly relativistic expanding HN and the rotational energy of the fast-rotating highly magnetized nu NS. We reproduce the afterglow in all wavelengths from the optical (10(14) Hz) to the X-ray band (10(19) Hz) over times from 604 s to 5.18 x 10(6) s relative to the Fermi-GBM trigger. Initially, the emission is dominated by the loss of kinetic energy of the HN component. After 105 s the emission is dominated by the loss of rotational energy of the nu NS, for which we adopt an initial rotation period of 2 ms and a dipole plus quadrupole magnetic field of less than or similar to 7 x 10(12) G or similar to 10(14) G. This scenario with a progenitor composed of a COcore and an NS companion differs from the traditional ultra-relativistic-jetted treatments of the afterglows originating from a single black hole.
Keywords:
binaries: general
black hole physics
gamma-ray burst: general
hydrodynamics
stars: neutron supernovae: general
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