Inferences from GRB 190114C: Magnetic Field and Afterglow of BdHN

Jorge A. Rueda, R. Ruffini, M. Karlica, R. Moradi, Y. Wang

Published 2019-05-27Version 1

GRB 190114C is the first binary-driven hypernova (BdHN) fully observed from the initial supernova (SN) shockwave breakout to the eventual emergence of the optical SN signal. It offers an unprecedented support for the BdHN theory. BdHNe comprise four subclasses of long gamma-ray bursts (GRBs) with progenitors as a binary system composed of a carbon-oxygen star (CO$_\textrm{core}$) and a neutron star (NS) or a black hole (BH) companion. The CO$_\textrm{core}$ explodes as a supernova (SN) leaving at its center a new NS ($\nu$NS). The SN hypercritically ejecta accretes onto the NS/BH companion. BdHNe I are the tightest binaries where the accretion leads the initial NS gravitationally collapses to a BH. In BdHN II the accretion onto the NS is lower, there is no BH formation. We infer for GRB 190114C and other selected examples of BdHN I (GRB 130427A, GRB 160509A, GRB 160625B), BdHN II (GRB 180728A) the intensity and structure of the $\nu$NS magnetic field needed for the explanation of the afterglow via synchrotron emission powered by the newborn NS. In the case of the BdHNe I, we infer as well the properties of the magnetic field around the newborn BH, requested for the explanation of the observed GeV emission through what we have called the ``inner engine'': the rotating BH surrounded by a magnetic field and matter from the SN ejecta. We also discuss the possible nature of the magnetic field both the one of the $\nu$NS and the one around the newborn BH.