\begin{document}$ c/\sqrt{3} $\end{document}) as the density increases. By increasing the strengths of the confinement parameter D and perturbation parameter C, the tendency for v to approach the extreme relativistic limit at high density is slightly weakened. For (proto-)strange stars, the novel quark mass scaling can accommodate massive proto-strange stars with their maximum mass surpassing twice the solar mass by considering the isentropic stages along the star evolution line, where the entropy per baryon of the star matter is set to be 0.5 and 1 with the lepton fraction \begin{document}$ Y_{l} $\end{document} = 0.4."> Strange quark matter and proto-strange stars in a baryon density-dependent quark mass model -
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