The white dwarf binary merger model of GRB 170817A

Abstract

Following the GRB 170817A prompt emission lasting a fraction of a second, 10 8 s of data in the X-rays, optical, and radio wavelengths have been acquired. We here present a model that fits the spectra, flux, and time variability of all these emissions, based on the thermal and synchrotron cooling of the expanding matter ejected in a binary white dwarf merger. The 10 −3 M of ejecta, expanding at velocities of 10 9 cm s −1 , are powered by the newborn massive, fast rotating, magnetized white dwarf with a mass of 1.3M , a rotation period of 12 s, and a dipole magnetic field ∼ 10 10 G, born in the merger of a 1.0+0.8M white dwarf binary. Therefore, the long-lasting mystery of the GRB 170817A nature is solved by the merger of a white dwarf binary that also explains the prompt emission energetics.

On the X-ray, optical and radio afterglows of the BdHN I GRB 180720B generated by the synchrotron emission

“…10 0 10 1 10 2 10 3 10 4 10 5 10 6 10 7 Time (s) First, we find the evolution of a generic electron injected at time t = t i with energy E i . Equation ( 3) can be integrated analytically leading to the energy evolution (Rueda 2022;Rueda et al 2022)…”