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- W2960412128 abstract "The AT2017gfo kilonova (kN) counterpart of the binary neutron star merger event GW170817 was characterized by an early-time bright peak in optical and UV bands. Such blue kN is commonly interpreted as a signature of weak r-process nucleosynthesis in a fast expanding wind whose origin is currently debated. Numerical relativity simulations with microphysical equations of state, approximate neutrino transport, and turbulent viscosity reveal a new hydrodynamics-driven mechanism that can power the blue kN. Spiral density waves in the remnant generate a characteristic wind of mass ∼10−2 and velocity ∼0.2 c. The ejected material has an electron fraction mostly distributed above 0.25 being partially reprocessed by hydrodynamic shocks in the expanding arms. The combination of dynamical ejecta and spiral-wave wind can account for solar system abundances of r-process elements and early-time observed light curves." @default.
- W2960412128 created "2019-07-23" @default.
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- W2960412128 date "2019-11-27" @default.
- W2960412128 modified "2023-10-16" @default.
- W2960412128 title "Spiral-wave Wind for the Blue Kilonova" @default.
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- W2960412128 doi "https://doi.org/10.3847/2041-8213/ab5794" @default.
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