\begin{document}$p=\zeta\rho+2\epsilon V_{\rm rot}^{2}\,\rho$\end{document}, where p and \begin{document}$\rho$\end{document} represent the pressure and density, respectively, \begin{document}$V_{\rm rot}$\end{document} depicts the rotation velocity of galaxy, and \begin{document}$\zeta$\end{document} and \begin{document}$ \epsilon$\end{document} are positive constants. It can obtain a density profile that is similar to the pseudo-isothermal halo model when \begin{document}$\epsilon$\end{document} is approximately 0.15. To obtain a more universally used model, let the equation of state include the polytropic model, i.e. \begin{document}$p= \frac{\zeta}{\rho_{0}^{s}}\rho^{1+s}+ 2\epsilon V_{\rm rot}^{2}\,\rho$\end{document}, from which we can obtain other types of density profiles, such as the profile that is nearly same as the Burkert profile, where s and \begin{document}$\rho_{0}$\end{document} are positive constants."> The possible equation of state of dark matter in low surface brightness galaxies -
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