Abstract
AbstractWe performed the comparison of three different numerical codes for constructing equilibrium models; (I) a code for static equilibrium configurations, (II) an implementation of the Hartle–Thorne slow‐rotation approximation, (III) a numerical solution of the full Einstein equations by LORENE. We aimed to construct sequences of uniformly rotating configurations at various rotation frequencies up to the Keplerian frequency for a hybrid hadronic–quark matter EOS where a smooth transition is provided between two separate phases. We investigated the difference between the results computed by the implementation of Hartle–Thorne slow‐rotation approximation and by LORENE/nrotstar, respectively. We have concluded that the codes can increase the difference between the slow‐rotating and the fast‐rotating approach exponentially, reaching 6.67% for the maximal mass configuration rotating at the Keplerian frequency.
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