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Maximum mass of axisymmetric rotating quark stars
Author(s) -
Zhou E.,
Tsokaros A.,
Rezzolla L.,
Xu R.
Publication year - 2017
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201713432
Subject(s) - physics , quark star , neutron star , equation of state , stars , strange matter , compact star , rotational symmetry , astrophysics , exotic star , pulsar , star (game theory) , quark , particle physics , mechanics , quantum mechanics
The internal structure of pulsar‐like compact stars is still a puzzle, as the equation of state ( EoS ) of cold dense matter is unclear yet. One way to distinguish between different EoSs of compact stars is based on the maximum mass of different EoSs , which can be estimated by solving the Tolman–Oppenheimer–Volkoff ( TOV ) equation. In a more realistic consideration, rotations should to be taken into account when estimating the maximum mass. It has been shown that rotating neutron stars could support up to 20% more mass compared with the TOV maximum mass ( M TOV ). However, apart from neutron star models, other models such as the quark star or the hybrid star model are also suggested as possible EoSs for compact stars. In this work, we apply numerical relativity calculation for axisymmetric rotating quark stars and investigate the solution sequences. We consider both the conventional MIT Bag model and another stiff EoS (strangeon star model) in our calculations. We find that rotating quark stars, different from rotating neutron stars, can support up to roughly 40% more mass than M TOV . Possible astrophysical influence and possible ways to distinguish between EoSs are discussed.