A first-principles binary neutron star merger model of GW170817, GRB170817A, and AT2017gfo

@misc{kiuchi2026firstprinciples,
  title = {{A first-principles binary neutron star merger model of GW170817, GRB170817A, and AT2017gfo}},
  author = {Kenta Kiuchi and Sho Fujibayashi and Kota Hayashi and Kyohei Kawaguchi and Quentin Pognan and Alexis Reboul-Salze and Yuichiro Sekiguchi and Masaru Shibata and Shinya Wanajo},
  howpublished = {arXiv},
  year = {2026},
  month = aug,
  doi = {10.48550/arxiv.2608.27555},
  eprint = {2608.27555},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2608.27555},
  note = {CC BY-SA 4.0},
}

TY  - UNPB
TI  - A first-principles binary neutron star merger model of GW170817, GRB170817A, and AT2017gfo
AU  - Kenta Kiuchi
AU  - Sho Fujibayashi
AU  - Kota Hayashi
AU  - Kyohei Kawaguchi
AU  - Quentin Pognan
AU  - Alexis Reboul-Salze
AU  - Yuichiro Sekiguchi
AU  - Masaru Shibata
AU  - Shinya Wanajo
PY  - 2026
DA  - 2026/08/27
PB  - arXiv
DO  - 10.48550/arxiv.2608.27555
UR  - https://arxiv.org/abs/2608.27555
AB  - The multimessenger observation of the binary neutron star merger event GW170817, associated with its electromagnetic counterparts GRB170817A and AT2017gfo, marked a milestone in astrophysics, yet its unified physical explanation remains elusive. We conduct an end-to-end simulation based on a first-principles general-relativistic magnetohydrodynamics neutrino-radiation transfer merger simulation, followed by nucleosynthesis calculations and photon radiative transfer to generate kilonova light curves. We show that the large-scale dynamo simultaneously produces a relativistic jet with an isotropic-equivalent luminosity of ∼ 10^51 erg s^−1 and ≈ 0.08M_⊙ of neutron-rich ejecta, reproducing the GRB170817A afterglow and the AT2017gfo kilonova light curves. Our results establish a unified first-principles framework for interpreting binary neutron star mergers across gravitational wave, gamma-ray burst, and kilonova observations.
ER  -