  We examine whether stellar flyby simulations can initiate FU Orionis
outbursts using 3D hydrodynamics simulations coupled to live Monte Carlo
radiative transfer. We find that a flyby where the secondary penetrates the
circumprimary disc triggers a 1-2 year rise in the mass accretion rate to
$10^{-4}~{\rm M_{\odot}~ yr^{-1}}$ that remains high ($\gtrsim 10^{-5}~{\rm
M_{\odot}~yr^{-1}}$) for more than a hundred years, similar to the outburst
observed in FU Ori. Importantly, we find that the less massive star becomes the
dominant accretor, as observed.
