Abstract
Abstract We perform multiwavelength light-curve modeling of the recently discovered low-luminosity gamma-ray burst (GRB) 171205A. The emission model is based on the relativistic ejecta–circumstellar medium (CSM) interaction scenario. The collision of freely expanding spherical ejecta traveling at mildly relativistic velocities with the CSM produces the reverse and forward shocks, which dissipate a part of the kinetic energy of the mildly relativistic ejecta. We show that the early gamma-ray emission followed by an X-ray tail can be well explained by the radiation diffusing out from the shocked gas. Mildly relativistic ejecta with a kinetic energy of 5 × 1050 erg and a wind-like CSM with a mass-loss rate of a few 10−4 M ⊙ yr−1 for a wind velocity of 103 km s−1, which extends up to ∼3 × 1013 cm, are required to account for the gamma-ray luminosity and duration of GRB 171205A. We also calculate the photospheric and nonthermal emission after the optically thick stage, which can fit the late-time X-ray, optical, and radio light curves. Our results suggest that the relativistic ejecta–CSM interaction can be a potential power source for low-luminosity GRBs and other X-ray-bright transients.
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