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Water ice is important for the evolution and preservation of life.Identifying the distribution of water ice in debris disks is therefore of greatinterest in the field of astrobiology. Furthermore, icy dust grains areexpected to play important roles throughout the entire planet formationprocess. However, currently available observations only allow deriving weakconclusions about the existence of water ice in debris disks. We investigatewhether it is feasible to detect water ice in typical debris disk systems. Wetake the following ice destruction mechanisms into account: sublimation of ice,dust production through planetesimal collisions, and photosputtering byUV-bright central stars. We consider icy dust mixture particles with variousshapes consisting of amorphous ice, crystalline ice, astrosilicate, and vacuuminclusions. We calculated optical properties of inhomogeneous icy dust mixturesusing effective medium theories, that is, Maxwell-Garnett rules. Subsequently,we generated synthetic debris disk observables, such as spectral energydistributions and spatially resolved thermal reemission and scattered lightintensity and polarization maps with our code DMS. We find that the prominent$\sim$ 3 $\mu\rm{m}$ and 44 $\mu\rm{m}$ water ice features can be potentiallydetected in future observations of debris disks with the James Webb SpaceTelescope and the Space Infrared telescope for Cosmology and Astrophysics. Weshow that the sublimation of ice, collisions between planetesimals, andphotosputtering caused by UV sources clearly affect the observationalappearance of debris disk systems. In addition, highly porous ice tends toproduce highly polarized radiation at around 3 $\mu\rm{m}$. Finally, thelocation of the ice survival line is determined by various dust properties suchas a fractional ratio of ice versus dust, physical states of ice, and theporosity of icy grains.

Constraining the detectability of water ice in debris disks