Rapidly rotating neutron stars with realistic nuclear matter equation of state

Abstract: We 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.

Angaben zum Objekt

• Standort: Deutsche Nationalbibliothek Frankfurt am Main
• Umfang: Online-Ressource
• Sprache: Englisch

Verweise und Beziehungen

• Erschienen in: Rapidly rotating neutron stars with realistic nuclear matter equation of state ; volume:344 ; number:1-2 ; year:2023 ; extent:6 ; Astronomische Nachrichten ; 344, Heft 1-2 (2023) (gesamt 6)

Beteiligte, Orts- und Zeitangaben

• Urheber: Kacskovics, Balázs ; Barta, Dániel ; Vasúth, Mátyás

Weitere Informationen

• DOI: 10.1002/asna.20220109
• URN: urn:nbn:de:101:1-2023033015054424847416
• Rechteinformation: Open Access; Der Zugriff auf das Objekt ist unbeschränkt möglich.
• Letzte Aktualisierung: 14.08.2025, 11:03 MESZ