\begin{document}$ \beta $\end{document} equilibrium. The four chemical potentials, \begin{document}$ \mu_u $\end{document}, \begin{document}$ \mu_d $\end{document}, \begin{document}$ \mu_s $\end{document} and \begin{document}$ \mu_e $\end{document}, are constrained by three conditions, so that one independent variable remains: we choose the average quark chemical potential as the free variable. All quark masses and number densities suffer discontinuities at the phase transition point. The strange quarks appear after the phase transition since the system needs more energy to produce a \begin{document}$ d $\end{document}-quark than an \begin{document}$ s $\end{document}-quark. Taking the EOS as an input, the TOV equations are solved numerically, and we show that the mass–radius relation is sensitive to the EOS. The maximum mass of strange quark stars is not susceptible to the parameter \begin{document}$ \Lambda_q $\end{document} we introduced."> Phase structures of neutral dense quark matter and applicationto strange stars -
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