Accuracy and Applicability of the Hartle–Thorne and Komatsu–Eriguchi–Hachisu Methods for Modeling Rotating Neutron Stars
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Le résumé fourni par la source
Abstract Neutron stars, which are composed of extremely dense nuclear matter, serve as natural laboratories to study nuclear interactions beyond the terrestrial experiments. Recent studies have actively explored how the equation of state (EoS) can be constrained by observed neutron star masses and radii, and how nuclear interactions affect their macroscopic properties. Most of these studies, however, rely on the Tolman–Oppenheimer–Volkoff (TOV) equations, which assumed static, spherically symmetric neutron stars. Since neutron stars are rotating objects and thus axisymmetrically deformed, the TOV calculation may be insufficient to capture their realistic structure. In this work, we investigate the influence of nuclear matter properties on the physical quantities of rotating neutron stars using two approaches: the perturbative Hartle–Thorne (HT) method and fully general relativistic Komatsu–Eriguchi–Hachisu (KEH) method. For nuclear EoS parameter sets, we examine the OMEG series, in which the slope of the symmetry energy L is systematically varied. We find that rotational effects lead to a noticeable increase in the stellar radius, which depends sensitively on values of L . Additionally, focusing on the rotational deformation, we show that the results obtained by these two methods deviate from each other even for the slowly rotating case, such as f = 200 Hz. These results reveal that, for detailed discussions on the internal structure and stability of rotating neutron stars, the fully general relativistic method, such as KEH, is indispensable.
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Le contrôle bibliographique ouvert
DOI retrouvé dans Crossref DOI retrouvé ; titre concordant.
- Titre Crossref
- Accuracy and Applicability of the Hartle–Thorne and Komatsu–Eriguchi–Hachisu Methods for Modeling Rotating Neutron Stars
- Date Crossref
- 02/04/2026
- Éditeur
- American Astronomical Society
- Type
- journal-article
Ce recoupement confirme des métadonnées liées au DOI. Il ne confirme ni la méthode ni les conclusions de l’étude, et il ne compte pas comme une seconde source scientifique indépendante.
Où se fait cette recherche
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Tokyo Institute of Technology pays non établi dans la noticeUniversité ou école supérieure
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Tokyo University of Science pays non établi dans la noticeUniversité ou école supérieure
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Soongsil University Department of Physics and Origin of Matter and Evolution of Galaxies Institute pays non établi dans la noticeUniversité ou école supérieure
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University of Tsukuba Center for Computational Sciences pays non établi dans la noticeUniversité ou école supérieure
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RIKEN Nishina Center pays non établi dans la noticeStructure de recherche
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School of Science Department of Physics pays non établi dans la noticeUniversité ou école supérieure
Tokyo Institute of Technology, Tokyo University of Science et Department of Physics and Origin of Matter and Evolution of Galaxies Institute — Soongsil University, avec 3 autres affiliations.
Une affiliation ne permet pas de déduire la nationalité d’un auteur.