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We perform the first 3D ab-initio general-relativistic neutrino-radiationhydrodynamics of a long-lived neutron star merger remnant spanning a fractionof its cooling time scale. We find that neutrino cooling becomes the dominantenergy loss mechanism after the gravitational-wave dominated phase (${\sim}20\{\rm ms}$ postmerger). Electron flavor anti-neutrino luminosity dominates overelectron flavor neutrino luminosity at early times, resulting in a secularincrease of the electron fraction in the outer layers of the remnant. However,the two luminosities become comparable ${\sim}20{-}40\ {\rm ms}$ postmerger. Adense gas of electron anti-neutrinos is formed in the outer core of the remnantat densities ${\sim}10^{14.5}\ {\rm g}\ {\rm cm}^{-3}$, corresponding totemperature hot spots. The neutrinos account for ${\sim}10\%$ of the leptonnumber in this region. Despite the negative radial temperature gradient, theradial entropy gradient remains positive and the remnant is stably stratifiedaccording to the Ledoux criterion for convection. A massive accretion disk isformed from the material squeezed out of the collisional interface between thestars. The disk carries a large fraction of the angular momentum of the system,allowing the remnant massive neutron star to settle to a quasi-steadyequilibrium within the region of possible stable rigidly rotatingconfigurations. The remnant is differentially rotating, but it is stableagainst the magnetorotational instability. Other MHD mechanisms operating onlonger timescales are likely responsible for the removal of the differentialrotation. Our results indicate the remnant massive neutron star is thusqualitatively different from a protoneutron stars formed in core-collapsesupernovae.

astrophysical journal/the astrophysical journal

Ab-Initio General-Relativistic Neutrino-Radiation Hydrodynamics  Simulations of Long-Lived Neutron Star Merger Remnants to Neutrino Cooling  Timescales