  FU Orionis-type objects(FUors) are embedded protostars that undergo episodes
of high accretion, potentially indicating a widespread but poorly understood
phase in the formation of low-mass stars. Gaining a better understanding of the
influence exerted by these outbursts on the evolution of the surrounding
protoplanetary disc may hold significant implications for the process of planet
formation and the evolution of disc chemistry. The heating due to outbursts of
high accretion in FUors pushes the snowlines of key volatiles farther out in
the disc, so they become easier to observe and study. Among the known FUors,
V883 Ori is of particular interest. V883 Ori was the first FUor to show
indirect evidence of a resolvable snowline beyond 40 au. By introducing a
radial-dependent model of this source including viscous heating, we show that
active heating is needed to reproduce the steep thermal profile of dust in the
inner disc of V883 Ori. Our disc modeling combines the effect of stellar
irradiation and the influence on the disc shape caused by the outburst of
accretion. The accuracy of our model is tested by comparing synthetic ALMA
images with continuum observations of V883 Ori, showing that the model
successfully reproduces the 1.3 mm emission of V883 Ori at high spatial
resolution. Our final predictions underline the importance of viscous heating
as a predominant heat source for this type of object, changing the physical
conditions (shape and temperature) of the disc, and influencing its evolution.
