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GW190425 was the second gravitational wave (GW) signal compatible with abinary neutron star (BNS) merger detected by the Advanced LIGO and AdvancedVirgo detectors. Since no electromagnetic counterpart was identified, whetherthe associated kilonova was too dim or the localisation area too broad is stillan open question. We simulate 28 BNS mergers with the chirp mass of GW190425and mass ratio $1 \leq q \leq 1.67$, using numerical-relativity simulationswith finite temperature, composition dependent nuclear equation of state (EOS)and neutrino radiation. The energy emitted in GWs is $\lesssim 0.083 M_{\odot}c^2$ with peak luminosity of $1.1-2.4 \times 10^{58} {\rm erg~s^{-1}}/(1+q)^2$.Dynamical ejecta and disc mass range between $5 \times 10^{-6} - \sim10^{-3}~M_{\odot}$ and $10^{-5} - 0.1~M_{\odot}$, respectively. Asymmetricmergers, especially with stiff EOS, unbind more matter and to form heavierdiscs compared to equal mass binaries. The angular momentum of the disc is$8-10 M_{\odot}~GM_{\rm disc}/c$ over three orders of magnitude in $M_{\rmdisc}$. While the nucleosynthesis shows no peculiarity, the simulated kilonovaeare relatively dim compared with the GW170817 event. For distances compatiblewith GW190425, AB magnitudes are always dimmer than $\sim20~{\rm mag}$ for the$B$, $r$ and $K$ bands, with brighter kilonovae associated to more asymmetricbinaries and stiffer EOS. We suggest that, even assuming a good coverage ofGW190425's sky location, the kilonova could hardly have been detected bypresent wide-field surveys and no firm constraints on the binary parameters orEOS can be argued from the lack of the detection.

Numerical relativity simulations of the neutron star merger GW190425: microphysics and mass ratio effects