Very-high-energy Gamma-Ray Afterglows of GRB 201015A and GRB 201216C

Gamma-ray bursts (GRBs) 201015A and 201216C are valuable cases where very-high-energy (VHE) gamma-ray afterglows have been detected. By analyzing their prompt emission data, we find that GRB 201216C is an extremely energetic, long GRB with a hard gamma-ray spectrum, while GRB 201015A is a relative subenergetic, soft-spectrum GRB. Attributing their radio-optical-X-ray afterglows to the synchrotron radiation of the relativistic electrons accelerated in their jets, we fit their afterglow lightcurves with the standard external shock model and infer their VHE afterglows from the synchrotron self-Compton scattering process of the electrons. It is found that the jet of GRB 201015A is midrelativistic (& UGamma;(0) = 44), surrounded by a very dense medium (n = 1202 cm(-3)), and the jet of GRB 201216C is ultrarelativistic (& UGamma;(0) = 331), surrounded by a moderate dense medium (n = 5 cm(-3)). The inferred peak luminosity of the VHE gamma-ray afterglows of GRB 201216C is approximately 10(-9) erg cm(-2) s(-1) at 57-600 s after the GRB trigger, making it detectable with the MAGIC telescopes at a high confidence level, even though the GRB is at a redshift of 1.1. Comparing their intrinsic VHE gamma-ray lightcurves and spectral energy distributions with GRBs 180720B, 190114C, and 190829A, we show that their intrinsic peak luminosity of VHE gamma-ray afterglows at 10(4) s after the GRB trigger is variable from 10(45) to 5 x 10(48) erg s(-1), and their kinetic energy, initial Lorentz factor, and medium density are diverse among bursts.