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A multi-messenger, black hole (BH) - neutron star (NS) merger event stillremains to be detected. The tidal (dynamical) ejecta from such an event,thought to produce a kinonova, is concentrated in the equatorial plane andoccupies only part of the whole azimuthal angle. In addition, recentsimulations suggest that the outflow or wind from the post-merger remnant disk,presumably anisotropic, can be a major ejecta component responsible for akilonova. For any ejecta whose photosphere shape deviates from the sphericalsymmetry, the electron scattering at the photosphere causes a net polarizationin the kilonova light. Recent observational and theoretical polarizationstudies have been focused to the NS-NS merger kilonova AT2017gfo. We extendthose work to the case of a BH-NS merger kilonova. We show that the degree ofpolarization at the first $\sim 1$ hr can be up to $\sim$ 3\% if a small amount($10^{-4} M_{\odot}$) of free neutrons have survived in the fastest componentof the dynamical ejecta, whose beta-decay causes a precursor in the kilonovalight. The polarization degree can be $\sim$ 0.6\% if free neutrons survived inthe fastest component of the disk wind. Future polarization detection of akilonova will constrain the morphology and composition of the dominant ejectacomponent, therefore help to identify the nature of the merger.

Polarization of kilonova emission from a black hole-neutron star merger