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Dwarf galaxies (M*<10^9 Msun) are key drivers of mass assembly in high massgalaxies, but relatively little is understood about the assembly of dwarfgalaxies themselves. Using the \textsc{NewHorizon} cosmological simulation (40pc spatial resolution), we investigate how mergers and fly-bys drive the massassembly and structural evolution of around 1000 field and group dwarfs up toz=0.5. We find that, while dwarf galaxies often exhibit disturbed morphologies(5 and 20 per cent are disturbed at z=1 and z=3 respectively), only a smallproportion of the morphological disturbances seen in dwarf galaxies are drivenby mergers at any redshift (for 10^9 Msun, mergers drive only 20 per centmorphological disturbances). They are instead primarily the result ofinteractions that do not end in a merger (e.g. fly-bys). Given the largefraction of apparently morphologically disturbed dwarf galaxies which are not,in fact, merging, this finding is particularly important to future studiesidentifying dwarf mergers and post-mergers morphologically at intermediate andhigh redshifts. Dwarfs typically undergo one major and one minor merger betweenz=5 and z=0.5, accounting for 10 per cent of their total stellar mass. Mergerscan also drive moderate star formation enhancements at lower redshifts (3 or 4times at z=1), but this accounts for only a few per cent of stellar mass in thedwarf regime given their infrequency. Non-merger interactions drivesignificantly smaller star formation enhancements (around two times), but theirpreponderance relative to mergers means they account for around 10 per cent ofstellar mass formed in the dwarf regime.

The role of mergers and interactions in driving the evolution of dwarf galaxies over cosmic time