  Since the derivation of a well-defined $D\rightarrow 4$ limit for 4
dimensional Einstein Gauss-Bonnet (4DEGB) gravity coupled to a scalar field,
there has been interest in testing it as an alternative to Einstein's general
theory of relativity. Using the Tolman-Oppenheimer-Volkoff (TOV) equations
modified for charge and 4DEGB gravity, we model the stellar structure of
charged, non-interacting quark stars. We find that increasing the Gauss-Bonnet
coupling constant $\alpha$ or the charge $Q$ both tend to increase the
mass-radius profiles of quark stars described by this theory, allowing a given
central pressure to support larger quark stars in general. We also derive a
generalization of the Buchdahl bound for charged stars in 4DEGB gravity. As in
the uncharged case, we find that quark stars can exist below the general
relativistic Buchdahl bound (BB) and Schwarzschild radius $R=2M$, due to the
lack of a mass gap between black holes and compact stars in the 4DEGB theory.
Even for $\alpha$ well within current observational constraints, we find that
quark star solutions in this theory can describe Extreme Compact Charged
Objects (ECCOs), objects whose radii are smaller than what is allowed by
general relativity.
