Speaker
Description
We estimate the neutrino emission from the decay chain of the $\pi$-meson and $\mu$-lepton, produced by proton-proton inelastic scattering in energetic ($E_{\rm iso}\geq 10^{52}$ erg) long gamma-ray bursts (GRBs), within the type I binary-driven hypernova (BdHN) model. The BdHN I progenitor is a binary system composed of a carbon-oxygen star (CO$_{\rm core}$) and a neutron star (NS) companion. The CO$_{\rm core}$ explosion as supernova (SN) triggers a massive accretion process onto the NS. For short orbital periods of few minutes, the NS reaches the critical mass, hence forming a black hole (BH). Recent numerical simulations of the above scenario show that the SN ejecta becomes highly asymmetric, creating a \textit{cavity} around the newborn BH site, due to the NS accretion and gravitational collapse. Therefore, the electron-positron ($e^{\pm}$) plasma created in the BH formation, during its isotropic and self-accelerating expansion, engulfs different amounts of ejecta baryons along different directions, leading to a direction-dependent Lorentz factor. The protons engulfed inside the high-density ($\sim 10^{23}$ particle/cm$^3$) ejecta reach energies in the range $1.24\leq E_p\leq 6.14$~GeV and interact with the unshocked protons in the ejecta. The protons engulfed from the low density region around the BH reach energies $\sim 1$~TeV and interact with the low-density ($\sim1$ particle/cm$^3$) protons of the interstellar medium (ISM). The above interactions give rise, respectively, to neutrino energies $E_{\nu}\leq 2$ GeV and $10\leq E_{\nu}\leq 10^3$ GeV, and for both cases we calculate the spectra and luminosity.
