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Recent numerical simulations in general relativistic magnetohydrodynamics(GRMHD) provide useful constraints for the interpretation of the GW170817discovery. Combining the observed data with these simulations leads to a boundon the maximum mass of a cold, spherical neutron star (the TOV limit): ${M_{\rmmax}^{\rm sph}}\lesssim 2.74/\beta$, where $\beta$ is the ratio of the maximummass of a uniformly rotating neutron star (the supramassive limit) over themaximum mass of a nonrotating star. Causality arguments allow $\beta$ to be ashigh as $1.27$, while most realistic candidate equations of state predict$\beta$ to be closer to $1.2$, yielding ${M_{\rm max}^{\rm sph}}$ in the range$2.16-2.28 M_\odot$. A minimal set of assumptions based on these simulationsdistinguishes this analysis from previous ones, but leads to a similarestimate. There are caveats, however, and they are enumerated and discussed.The caveats can be removed by further simulations and analysis to firm up thebasic argument.

GW170817, General Relativistic Magnetohydrodynamic Simulations, and the Neutron Star Maximum Mass