  Investigating the response of icy dust aggregates to water ice sublimation is
essential for understanding the formation and properties of planetesimals in
protoplanetary discs. However, their fate remains unclear, as previous studies
suggest aggregates could either survive or completely fall apart to
(sub){\mu}m-sized grains. Protoplanetary discs around stars undergoing
accretion outbursts represent a unique laboratory to study the ice sublimation
process, as the water snowline is pushed outward to regions accessible to
current observatories. In this work, we aim to understand the aggregates'
response to ice sublimation by focusing on V883 Ori, a system currently
undergoing a powerful accretion outburst. We present new analysis of archival
high resolution ALMA observations of the protoplanetary disc of V883 Ori at
0.88, 1.3, 2.0, and 3.1 mm, and derive new radial spectral index profiles,
which we compare with predictions from one-dimensional dust evolution
simulations. In the region of V883 Ori where water ice has sublimated, we find
lower spectral indices than previously obtained, indicating the presence of
cm-sized particles. Coupled with our dust evolution models, we find that the
only way to explain their presence is to assume they formed before the
outburst, and survived the sublimation process. The resilience of dust
aggregates to such intense events leads us to speculate that it may extend to
other environments with more gentle heating, such as pebbles drifting through
the water snowline in quiescent protoplanetary discs. In that case, it may
alter the formation pathway of dry planetesimals interior to the snowline.
