The observations of pulsars heavier than $2M_{\odot }$ have put strong constraints on the equation of state (EoS) above nuclear saturation density. For this reason, the internal structure of a neutron star which is strictly correlated with the EoS is an active area of investigation in theoretical astrophysics. Here, we investigate the possible sequels for the quark stars consisting of a homogeneous and unpaired charge-neutral 3-flavor interacting quark matter with $\mathcal{O}\left(m_s^4\right)$ corrections that accounts for the quark strong interactions. In particular, the quark stars (QSs) with a well-motivated quantum chromodynamics (QCD) EoS are presented in Einstein gravity with the Gauss–Bonnet (GB) combination of quadratic curvature terms. We analyze the dependence of the physical properties of these QSs on the Gauss–Bonnet coupling strength. In fact, the existence and stability of QSs depend on the effects of fourth-order corrections parameter ($a_4$) of the QCD perturbation. We also present and discuss the calculated results for mass–central mass density ($M$–${\rho }_c$) relation and also the mass–radius (M–R) relation of QSs. Nevertheless, such deviations may be observable in future astrophysical probes.

脉冲星的观测比 $\mathrm{2个}{\mathrm{中号}}_{\odot }$已经对高于核饱和密度的状态方程（EoS）施加了严格的约束。因此，与EoS严格相关的中子星内部结构是理论天体物理学研究的一个活跃领域。在这里，我们研究了夸克恒星的可能续集，这些恒星由均质且不成对的电荷中性3味相互作用夸克物质与$\mathcal{Ø}（{米}_s^4）$导致夸克强烈相互作用的更正。特别是，具有良好动机的量子色动力学（QCD）EoS的夸克星（QSs）以爱因斯坦引力和二次曲率项的高斯-邦尼特（GB）组合呈现。我们分析了这些QS的物理特性对高斯-贝奈特耦合强度的依赖性。实际上，QS的存在和稳定性取决于四阶校正参数（${\mathrm{一种}}_4$）的QCD扰动。我们还将介绍并讨论质量-中心质量密度的计算结果（$\mathrm{中号}$–${\rho }_C$）关系以及QS的质量半径（MR）关系。然而，在将来的天体探测中这种偏差可能是可观察到的。