End-to-end simulation reproduces GW170817 jet luminosity and 0.08 solar mass ejecta

Kiuchi and colleagues performed an end-to-end calculation starting from a magnetized neutron-star merger, evolving the system through large-scale dynamo amplification, jet launching, and nucleosynthesis, then post-processing photon radiative transfer for synthetic light curves. The model reproduces the observed short gamma-ray burst energetics and the multi-band kilonova evolution without tunable parameters beyond the initial binary configuration. The result supplies the first unified, ab-initio account of the three messengers from GW170817. Prior analytic or semi-analytic models required separate prescriptions for jet power and ejecta mass; here both emerge from the same dynamo-driven outflow, tightening constraints on the neutron-star equation of state and r-process yields. Heavy-element production estimates derived from the 0.08 solar-mass ejecta mass align with galactic chemical-evolution requirements once scaled to the local merger rate. The simulation also predicts a modest dependence of jet luminosity on remnant spin, offering a testable signature for the next LIGO-Virgo-KAGRA observing run. Next steps include higher-resolution runs that resolve small-scale turbulence and incorporation of neutrino flavor oscillations to refine abundance patterns; these refinements can be confronted with additional multimessenger events expected within the next two years.