REVIEW 5 cited by
Self-consistent picture of the mass ejection from a one second-long binary neutron star merger leaving a short-lived remnant in general-relativistic neutrino-radiation magnetohydrodynamic simulation
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
We perform a general-relativistic neutrino-radiation magnetohydrodynamic simulation of a one second-long binary neutron star merger on Japanese supercomputer Fugaku using about $72$ million CPU hours with $20,736$ CPUs. We consider an asymmetric binary neutron star merger with masses of $1.2$ and $1.5M_\odot$ and a `soft' equation of state SFHo. It results in a short-lived remnant with the lifetime of $\approx 0.017$\,s, and subsequent massive torus formation with the mass of $\approx 0.05M_\odot$ after the remnant collapses to a black hole. For the first time, we confirm that after the dynamical mass ejection, which drives the fast tail and mildly relativistic components, the post-merger mass ejection from the massive torus takes place due to the magnetorotational instability-driven turbulent viscosity and the two ejecta components are seen in the distributions of the electron fraction and velocity with distinct features.
Forward citations
Cited by 5 Pith papers
-
From Multimessenger Inference to Simulations: A Ranked Ensemble of Finite-Temperature Equations of State
The paper constructs a 12-member ensemble of finite-temperature neutron star equations of state that spans the posterior from multimessenger and nuclear-physics constraints and releases simulation-ready tables.
-
Subsolar-mass binary mergers of strange stars and neutron stars: gravitational waves and ejecta
Subsolar strange star mergers produce a lower post-merger-to-cutoff GW frequency ratio than neutron star mergers, cleanly separating the two classes across equations of state and mass ratios.
-
Transport Properties of the MRI in Differentially Rotating Neutron Stars
Saturated MRI turbulence in differentially rotating neutron stars yields ℓ_mix ≈ (0.01–0.1) λ_MRI, largely independent of density, so standard GRLES mixing-length prescriptions overestimate transport by about an order...
-
Magnetic Field Configurations in Binary Neutron Star Mergers II: Inspiral, Merger and Ejecta
Initial magnetic field topology, especially anti-aligned poloidal fields, strongly controls post-merger field amplification and ejecta magnetisation in neutron star merger simulations.
-
Neutrino pair annihilation driven jets from black-hole torus systems
Neutrino pair annihilation in black hole-torus systems launches relativistic fireballs with isotropic energies up to about 10^51 erg and durations around 0.1 s, which can account for faint short GRBs and GRB precursors.
Discussion (0). Sign in to comment.