  The properties of galaxies in low-density regions of the universe suggest an
interplay between galaxy formation and environment. However, the specific
reason why this particular large-scale environment influences the evolution of
galaxies remains unclear. This paper examines the properties and evolutionary
paths of galaxies within cosmic voids using the Illustris TNG300 simulation.
The population of void galaxies at z = 0 has a higher star formation rate, a
smaller stellar-to-halo-mass ratio, higher gas metallicity, and lower stellar
metallicity in comparison with non-void galaxies at fixed stellar mass. Our
analysis shows that these differences are mainly due to the characteristics of
galaxies classified as satellites, for which the largest differences between
void and non-void samples are found. Although the mean number of mergers is
similar between void and non-void samples at a fixed stellar mass, void
galaxies tend to experience mergers at later times, resulting in a more recent
accumulation of accreted stellar mass. While the mean net accreted mass is
comparable for high mass galaxies, low mass void galaxies tend to exhibit
higher fractions of accreted stars than non-void galaxies. This finding
challenges the common notion that void galaxies predominantly experience growth
with infrequent mergers or interactions.
