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On 2018 July 28, GRB 180728A triggered \textit{Swift} satellites and, soonafter the determination of the redshift, we identified this source as a type IIbinary-driven hypernova (BdHN II) in our model. Consequently, we predicted theappearance time of its associated supernova (SN), which was later confirmed asSN 2018fip. A BdHN II originates in a binary composed of a carbon-oxygen core(CO$_{\rm core}$) undergoing SN, and the SN ejecta hypercritically accrete ontoa companion neutron star (NS). From the time of the SN shock breakout to thetime when the hypercritical accretion starts, we infer the binary separation$\simeq 3 \times 10^{10}$ cm. The accretion explains the prompt emission ofisotropic energy $\simeq 3 \times 10^{51}$ erg, lasting $\sim 10$ s, and theaccompanying observed blackbody emission from a thermal convective instabilitybubble. The new neutron star ($\nu$NS) originating from the SN powers the lateafterglow from which a $\nu$NS initial spin of $2.5$ ms is inferred. We compareGRB 180728A with GRB 130427A, a type I binary-driven hypernova (BdHN I) withisotropic energy $> 10^{54}$ erg. For GRB 130427A we have inferred an initiallycloser binary separation of $\simeq 10^{10}$ cm, implying a higher accretionrate leading to the collapse of the NS companion with consequent black holeformation, and a faster, $1$ ms spinning $\nu$NS. In both cases, the opticalspectra of the SNe are similar, and not correlated to the energy of thegamma-ray burst. We present three-dimensional smoothed-particle-hydrodynamicsimulations and visualisations of the BdHNe I and II.

Two Predictions of supernova: GRB 130427A / SN 2013cq and GRB 180728A / SN 2018fip