On the rise times in FU Orionis events
  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.
