Spiral-wave Wind for the Blue Kilonova

Vsevolod Nedora, Sebastiano Bernuzzi, David Radice, Albino Perego, Andrea Endrizzi, Néstor Ortiz

Research output: Contribution to journalArticlepeer-review

12 Scopus citations

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 M· 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.

Original languageEnglish (US)
Article numberL30
JournalAstrophysical Journal Letters
Volume886
Issue number2
DOIs
StatePublished - Dec 1 2019

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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