The white dwarf binary merger model of GRB 170817A
arXiv:2202.00314 · doi:10.1142/S0218271822300130
Abstract
Following the GRB 170817A prompt emission lasting a fraction of a second, 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 of ejecta, expanding at velocities of cm s, are powered by the newborn massive, fast rotating, magnetized white dwarf with a mass of , a rotation period of s, and a dipole magnetic field G, born in the merger of a 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.
arXiv commentTo appear in the IJMPD. Plenary talk at the 16th Marcel Grossmann Meeting on Relativistic Astrophysics held on July 5-10, 2021
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