  The Universe is shaped as a web-like structure, formed by clusters,
filaments, and walls that leave large volumes in between named voids. Galaxies
in voids have been found to be of a later type, bluer, less massive, and to
have a slower evolution than galaxies in denser environments (filaments and
walls). However, the effect of the void environment on their stellar population
properties is still unclear. We aim to address this question using 118 optical
integral field unit datacubes from the Calar Alto Void Integral-field Treasury
surveY (CAVITY), observed with the PMAS/PPaK spectrograph at the 3.5m telescope
at the Calar Alto Observatory (Almer\'ia, Spain). We used the non-parametric
full spectral fitting code STARLIGHT to estimate their stellar population
properties: stellar mass, stellar mass surface density, age, star formation
rate (SFR), and specific star formation rate (sSFR). We analysed the results
through the global and spatially resolved properties. Then, we compared them
with a control sample of galaxies in filaments and walls from the CALIFA
survey, matched in stellar mass and morphological type. Key findings include
void galaxies having a slightly higher half-light radius (HLR), lower stellar
mass surface density, and younger ages across all morphological types, and
slightly elevated SFR and sSFR (only significant enough for Sas). Many of these
differences appear in the outer parts of spiral galaxies in voids (HLR > 1),
which are younger and exhibit a higher sSFR, indicative of less evolved discs.
This trend is also found for early-type spirals, suggesting a slower transition
from star-forming to quiescent states in voids. Our analysis indicates that
void galaxies, influenced by their surroundings, undergo a more gradual
evolution, especially in their outer regions, with a more pronounced effect for
low-mass galaxies.
