Research results and animations

2022

General-relativistic neutrino-radiation magnetohydrodynamic simulation of seconds-long black hole-neutron star mergers

© K. Hayashi (Kyoto University)

Numerical simulation of a black hole-neutron star merger

The left side of the simulation shows the density profile (blue and green contours) with the magnetic-field lines (pink curves) penetrating the black hole, unbound matter (white color) and its velocity (green arrows). The right side displays the magnetic-field strength (magenta) and magnetic-field lines (light-blue curves).

Publication:

2021

Properties of the remnant disk and the dynamical ejecta produced in low-mass black hole-neutron star mergers

© K. Hayashi (Yukawa Institute for Theoretical Physics, Kyoto University), M. Shibata (Max Planck Institute for Gravitational Physics & Yukawa Institute for Theoretical Physics, Kyoto University)

Merger of a low-mass black hole and neutron star leading to a black hole surrounded by an accretion disk

When a black hole (black sphere) and a neutron star (red sphere) merge, matter is ejected and forms an accretion disk surrounding the resulting black hole. The simulation shows the density of the ejected matter with colors ranging from blue (lower density), green, yellow to red (higher density).

Publication:

2020

Mass ejection from disks surrounding a low-mass black hole: Viscous neutrino-radiation hydrodynamics simulation in full general relativity

© S. Fujibayashi (Max Planck Institute for Gravitational Physics), M. Shibata (Max Planck Institute for Gravitational Physics & Yukawa Institute for Theoretical Physics, Kyoto University)

Viscous evolution of disks for M_disk = 0.1 M_⊙

Rest-mass density in units of g=cm³, temperature (kT) in units of MeV, specific entropy per baryon in units of k, and electron fraction Y_e for model K8. The rest-mass density, the value of Y_e, and the temperature of the  atmosphere artificially added are ≈10 g=cm³, 0.5, and ≈0.036 MeV=k, respectively.

Publication: