  Void galaxies are essential for understanding the physical processes that
drive galaxy evolution because they are less affected by external factors than
galaxies in denser environments, that is, in filaments, walls, and clusters.
The stellar metallicity of a galaxy traces the accumulated fossil record of the
star formation through the entire life of the galaxy. A comparison of the
stellar metallicity of galaxies in various environments, including voids,
filaments, walls, and clusters can provide valuable insights into how the
large-scale environment affects the chemical evolution of the galaxy. We
present the first comparison of the relation of the total stellar mass versus
central stellar metallicity between galaxies in voids, filaments, walls, and
clusters with different star formation history (SFH) types, morphologies, and
colours for stellar masses between $10^{8.0}$ to $10^{11.5}$ solar masses and
redshift $0.01<z<0.05$. We applied non-parametric full spectral fitting
techniques (pPXF and STECKMAP) to 10807 spectra from the SDSS-DR7 (987 in
voids, 6463 in filaments and walls, and 3357 in clusters) and derived their
central mass-weighted average stellar metallicity ($\rm [M/H]_M$). We find that
galaxies in voids have slightly lower stellar metallicities on average than
galaxies in filaments and walls (by~$\sim~0.1$~dex), and they are much lower
than those of galaxies in clusters (by~$\sim~0.4$~dex). These differences are
more significant for low-mass ($ \sim~10^{9.25}~{\rm M_\odot}$) than for
high-mass galaxies, for long-timescale SFH (extended along time) galaxies than
for short-timescale SFHs (concentrated at early times) galaxies, for spiral
than for elliptical galaxies, and for blue than for red galaxies.
