Ultrahigh Energy Cosmic Ray Production in Binary Neutron Star Mergers

We predict the spectrum and composition of ultrahigh energy cosmic rays (UCRs for short) generated in a binary neutron star merger, exploiting the highly constrained initial conditions to make quantitative predictions for the cutoff energy for various nuclei. The key mechanism producing UCRs heavier than helium is acceleration in the magnetized turbulent outflow outside the jets. We find the rigidity cutoff of this component is $\mathcal{R}_{\rm cut} \equiv E_{\rm cut}/eZ \approx 6-9$ EV, consistent with the measured value $\mathcal{R}_{\rm cut} = 6.8^{+5.8}_{-2.8}\,$EV from fitting data. This agreement strengthens the case that BNS mergers are the main site of UCR production. The jets may also be capable of accelerating particles to ultrahigh energy: these UCRs would be protons and/or helium, in a ratio that depends on the neutron star equation of state. We estimate the cutoff energies of such a component to be $E_{\rm cut}\approx\! 10\,$EeV for p and $\approx\! 30\,$EeV for He. Such a jet component may explain the hint of a secondary light population at higher energy found in the analysis of Muzio et al. (2019). With more precise data, the locus of production of helium and intermediate mass nuclei can be inferred from their rigidity structure, and the predicted small deviations from a pure Peters Cycle can be checked. Predicting the relative abundances of different elements and the total energy in UCRs per merger event is feasible, but beyond the scope of this paper. This scenario predicts that each neutrino above 1 PEV is co-directional with a gravitational wave arriving ~1 day earlier, and that the highest energy UCRs have masses heavier than iron.