A MESA grid of 338 helium-star plus 1.4 solar-mass neutron star binaries at solar metallicity produces only 0.01% of double neutron stars with total mass at or above 3 solar masses, implying that the unstable mass-transfer channel cannot explain GW190425.
P., et al., 2017a, Phys
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Formation of heavy double neutron stars I: Eddington-limited accretion for a 1.4 $M_{\odot}$ neutron star at solar metallicity
A MESA grid of 338 helium-star plus 1.4 solar-mass neutron star binaries at solar metallicity produces only 0.01% of double neutron stars with total mass at or above 3 solar masses, implying that the unstable mass-transfer channel cannot explain GW190425.