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We investigate the effects ultralight bosonic field dark matter may have onthe dynamics of unstable differentially-rotating neutron stars prone to thebar-mode instability. To this aim we perform numerical simulations in generalrelativity of rotating neutron stars accreting an initial spherically symmetricbosonic field cloud, solving the Einstein-(complex, massive) Klein-Gordon-Eulerand the Einstein-(complex) Proca-Euler systems. We find that the presence ofthe bosonic field can critically modify the development of the bar-modeinstability of neutron stars, depending on the total mass of the bosonic fieldand on the boson particle mass. In some cases, the accreting bosonic field caneven quench the dominant $\ell=m=2$ mode of the bar-deformation by dynamicallyforming a mixed (fermion-boson) star that retains part of the angular momentumof the original neutron star. However, the mixed star undergoes the developmentof a mixed bar that leads to significant gravitational-wave emission,substantially different to that of the isolated neutron star. Our resultsindicate that dark-matter accretion in neutron stars could change the frequencyof the expected emission of the bar-mode instability, which would have animportant impact on ongoing searches for continuous gravitational waves.

Impact of ultralight bosonic dark matter on the dynamical bar-mode instability of rotating neutron stars