Hayashi Kota, Kiuchi Kenta, Kyutoku Koutarou, Sekiguchi Yuichiro, Shibata Masaru
Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, Postdam-Golm 14476, Germany.
Yukawa Institute for Theoretical Physics, Center for Gravitational Physics and Quantum Information, Kyoto University, Kyoto 606-8502, Japan.
Phys Rev Lett. 2025 May 30;134(21):211407. doi: 10.1103/PhysRevLett.134.211407.
We performed the longest numerical-relativity neutrino-radiation magnetohydrodynamics simulation for a binary neutron star merger that extends to ≈1.5 s after the merger. We consider the binary model that undergoes the prompt collapse to a black hole after the merger with asymmetric mass 1.25M_{⊙} and 1.65M_{⊙} and SFHo equation of state. We find the Poynting flux-driven collimated outflow as well as the gravitational wave emission, neutrino emission, dynamical mass ejection, and postmerger mass ejection facilitated by magnetorotational instability-driven turbulent viscosity in a single self-consistent binary neutron star merger simulation. A magnetosphere dominated by the aligned global magnetic field penetrating the black hole develops along the black-hole spin axis after the turbulence in the remnant disk is enhanced. A jet with the Poynting flux with isotropic-equivalent luminosity of ∼10^{49} erg/s is launched, and the duration of the high luminosity is expected to be O(1) s.
