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FU Orionis-type objects(FUors) are embedded protostars that undergo episodesof high accretion, potentially indicating a widespread but poorly understoodphase in the formation of low-mass stars. Gaining a better understanding of theinfluence exerted by these outbursts on the evolution of the surroundingprotoplanetary disc may hold significant implications for the process of planetformation and the evolution of disc chemistry. The heating due to outbursts ofhigh accretion in FUors pushes the snowlines of key volatiles farther out inthe 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 showindirect evidence of a resolvable snowline beyond 40 au. By introducing aradial-dependent model of this source including viscous heating, we show thatactive heating is needed to reproduce the steep thermal profile of dust in theinner disc of V883 Ori. Our disc modeling combines the effect of stellarirradiation and the influence on the disc shape caused by the outburst ofaccretion. The accuracy of our model is tested by comparing synthetic ALMAimages with continuum observations of V883 Ori, showing that the modelsuccessfully reproduces the 1.3 mm emission of V883 Ori at high spatialresolution. Our final predictions underline the importance of viscous heatingas a predominant heat source for this type of object, changing the physicalconditions (shape and temperature) of the disc, and influencing its evolution.

Viscous heating as the dominant heat source inside the water snowline of V883 Ori