\begin{document}$\kappa$\end{document}. From this bound, we can constrain \begin{document}$\kappa\lesssim 10^{8}\;{\rm{m}}^2$\end{document} if a neutron star with a mass around \begin{document}$3M_{\odot}$\end{document} is observed in the future. In addition, to avoid the potential pathologies in EiBI, a Hagedorn-like equation of state associated with \begin{document}$\kappa$\end{document} at the center of a compact star is inevitable, which is similar to the Hagedorn temperature in string theory."> The Buchdahl stability bound in Eddington-inspired Born-Infeld gravity -
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