  We present gas-phase elemental abundance ratios of 7 local extremely
metal-poor galaxies (EMPGs) including our new Keck/LRIS spectroscopy
determinations together with 33 JWST $z\sim 4-10$ star-forming galaxies in the
literature, and compare chemical evolution models. We develop chemical
evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia
supernovae, hypernovae (HNe), and pair-instability supernovae (PISNe), and
compare the EMPGs and high-$z$ galaxies in conjunction with dust depletion
contributions. We find that high Fe/O values of EMPGs can (cannot) be explained
by PISN metal enrichments (CCSN/HN enrichments even with the
mixing-and-fallback mechanism enhancing iron abundance), while that the
observed Ar/O and S/O values are much smaller than the predictions of the PISN
models. The abundance ratios of the EMPGs can be explained by the combination
of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly
fallback, which are comparable with Sculptor stellar chemical abundance
distribution, suggesting that early chemical enrichment is taken place in the
EMPGs. Comparing our chemical evolution models with the star-forming galaxies
at $z\sim 4-10$, we find that the Ar/O and S/O ratios of the high-$z$ galaxies
are comparable with those of the CCSNe/HNe models, while majority of the
high-$z$ galaxies do not have constraints good enough to rule out contributions
from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained
even by rotating PISNe, but could be reproduced by the winds of rotating Wolf
Rayet stars that end up as a direct collapse.
