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We explore the stellar structure and radial stability of charged quark starscomposed of interacting quark matter (IQM) in three classes of commonly usedcharge models. We adopt a general parametrization of IQM equation of state thatincludes the corrections from perturbative QCD, color superconductivity, andthe strange quark mass into one parameter $\lambda$, or one dimensionlessparameter $\bar{\lambda}=\lambda^2/(4B_{\rm eff})$ after being rescaled withthe effective bag constant $B_{\rm eff}$. We find that increasing charge tendsto increase the mass and radius profiles, and enlarges the separation size inmass between the maximum mass point and the point where zero eigenfrequencies$\omega^2_0=0$ of the fundamental radial oscillation mode occur. The sign ofthe separation in central density depends on the charge model; this separationalso has a dependence on $\lambda$ such that increasing $\lambda$ (which canoccur for either large color superconductivity or small strange quark mass)tends to decrease this separation size for the first and third classes ofcharge models monotonically. Moreover, for the second and third classes ofcharge models, we manage to numerically and analytically identify a new kind ofstellar structure with a zero central pressure but a finite radius and mass.All the calculations and analysis are performed in a general dimensionlessrescaling approach so that the results are independent of explicit values ofdimensional parameters.

Stellar Structure and Stability of Charged Interacting Quark Stars and Their Scaling Behaviour