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The merging of a binary system involving two neutron stars (NSs), or a blackhole (BH) and a NS, often results in the emission of an electromagnetic (EM)transient. One component of this EM transient is the epic explosion known as akilonova (KN). The characteristics of the KN emission can be used to probe theequation of state (EoS) of NS matter responsible for its formation. We predictKN light curves from computationally simulated BH-NS mergers, by using the 3Dradiative transfer code \texttt{POSSIS}. We investigate two EoSs spanning mostof the allowed range of the mass-radius diagram. We also consider a soft EoScompatible with the observational data within the so-called 2-families scenarioin which hadronic stars coexist with strange stars. Computed results show thatthe 2-families scenario, characterized by a soft EoS, should not produce a KNunless the mass of the binary components are small ($M_{\rm BH} \leq6M_{\odot}$, $M_{\rm NS} \leq 1.4M_{\odot}$) and the BH is rapidly spinning($\chi_{\rm BH} \geq 0.3$). In contrast, a strong KN signal potentiallyobservable from future surveys (e.g. VRO/LSST) is produced in the 1-familyscenario for a wider region of the parameter space, and even for non-rotatingBHs ($\chi_{\rm BH} = 0$) when $M_{\rm BH} = 4M_{\odot}$ and $M_{\rm NS} =1.2M_{\odot}$. We also provide a fit that allows for the calculation of theunbound mass from the observed KN magnitude, without running timely and costlyradiative transfer simulations. Findings presented in this paper will be usedto interpret light curves anticipated during the fourth observing run (O4), ofthe advanced LIGO, advanced Virgo and KAGRA interferometers and thus toconstrain the EoS of NS matter.

Black Hole - Neutron Star mergers: using kilonovae to constrain the equation of state