  Disks around young stellar objects (YSOs) consist of material that thermally
emits the energy provided by a combination of passive heating from the central
star, and active, viscous heating due to mass accretion. FU Ori stars are YSOs
with substantially enhanced accretion rates in their inner disk regions. As a
disk transitions from standard low-state, to FU Ori-like high-state accretion,
the outburst manifests through photometric brightening over a broad range of
wavelengths. We present results for the expected amplitudes of the brightening
between $\sim$4000 \AA\ and 8 $\mu$m -- the wavelength range where FU Ori type
outburst events are most commonly detected. Our model consists of an optically
thick passive $+$ active steady-state accretion disk with low and high
accretion states.
