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Open AccessArticle

Rotating Quark Stars in General Relativity

1
State Key Laboratory of Nuclear Science and Technology and School of Physics, Peking University, Beijing 100871, China
2
Institute for Theoretical Physics, Frankfurt am Main 60438, Germany
3
Frankfurt Institute of Advanced Studies, 60438 Frankfurt am Main, Germany
4
Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA
5
Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China
6
Department of Physics, University of the Ryukyus, Senbaru, Nishihara, Okinawa 903-0213, Japan
*
Author to whom correspondence should be addressed.
Current address: State Key Laboratory of Nuclear Science and Technology and School of Physics, Peking University, Beijing 100871, China.
Universe 2018, 4(3), 48; https://doi.org/10.3390/universe4030048
Received: 4 January 2018 / Revised: 23 February 2018 / Accepted: 26 February 2018 / Published: 5 March 2018
(This article belongs to the Special Issue Compact Stars in the QCD Phase Diagram)
We have built quasi-equilibrium models for uniformly rotating quark stars in general relativity. The conformal flatness approximation is employed and the Compact Object CALculator (cocal) code is extended to treat rotating stars with surface density discontinuity. In addition to the widely used MIT bag model, we have considered a strangeon star equation of state (EoS), suggested by Lai and Xu, that is based on quark clustering and results in a stiff EoS. We have investigated the maximum mass of uniformly rotating axisymmetric quark stars. We have also built triaxially deformed solutions for extremely fast rotating quark stars and studied the possible gravitational wave emission from such configurations. View Full-Text
Keywords: pulsars; quark stars; general relativity pulsars; quark stars; general relativity
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MDPI and ACS Style

Zhou, E.; Tsokaros, A.; Rezzolla, L.; Xu, R.; Uryū, K. Rotating Quark Stars in General Relativity. Universe 2018, 4, 48.

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