QUARK MATTER IN MASSIVE COMPACT STARS

By S. Weissenborn, Irina Sagert, G. Pagliara, M. Hempel, J. Schaffner-Bielich. 2011

179 citations recorded by the source corpus.

The recent observation of the pulsar PSR J1614-2230 with a mass of 1.97 ± 0.04 M☉ gives a strong constraint on the quark and nuclear matter equations of state (EoS). We explore the parameter ranges for a parameterized EoS for quark stars. We find that strange stars, made of absolutely stable strange quark matter, comply with the new constraint only if effects from the strong coupling constant and color-superconductivity are taken into account. Hybrid stars, compact stars with a quark matter core and a hadronic outer layer, can be as massive as 2 M☉, but only for a significantly limited range of parameters. We demonstrate that the appearance of quark matter in massive stars crucially depends on the stiffness of the nuclear matter EoS. We show that the masses of hybrid stars stay below the ones of hadronic and pure quark stars, due to the softening of the EoS at the quark–hadron phase transition.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/f301c49171f23897e4a86caa7cb15fc46942110a

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In Astronomy and Astrophysics

1. A. Kurkela
2. A. Vuorinen
3. Y. Lim
4. J. Lattimer
5. E. Fraga
6. T. Hatsuda
7. P. Haensel
8. J. Zdunik

In Instrumentation

1. J. Lattimer

In Statistical and Nonlinear Physics

1. J. Lattimer
2. T. Hatsuda
3. Y. Lim
4. Luciano Rezzolla
5. C. Breu
6. T. Birnstiel

Citations in the corpus

• CONSTRAINING THE SYMMETRY PARAMETERS OF THE NUCLEAR INTERACTION (2012, background): “Weissenborn et al. (2011) have shown that the existence of hybrid quark stars with a mixed phase and having a sufficiently large maximum mass is strongly dependent upon the assumed hadronic EOS, and is limited to small, specific ranges of quark matter parameters.”
• Composition and stability of hybrid stars with hyperons and quark color-superconductivity (2011, methodology): “…the quark matter equation of state motivated by the MIT bag model in combination with nuclear equations of state that are moderately soft; large masses require strong quark-quark correlations in combinatio with color superconductivity in the CFL phase (Alford et al. 2005; Weissenborn et al. 2011).”
• Maximum mass of neutron stars and strange neutron-star cores (2012, background): “…of the discovery of a 2 M pulsar, several models of quark cores of NS (hybrid stars), with the necessary properties to yield Mmax > 2.0 M , have been proposed (Özel et al. 2010; Weissenborn et al. 2011; Klaehn et al. 2012; Bonanno & Sedrakian 2012; Łastowiecki et al. 2012; Lenzi & Lugones 2012).”
• INTERACTING QUARK MATTER EQUATION OF STATE FOR COMPACT STARS (2013, background): “…of high density and low temperature, common wisdom based on the MIT bag model EOS states that the masses of pure quark stars are unlikely to reach 2 M , and hybrid stars containing quark matter cores are generically less massive than their purely nucleonic counterparts (Weissenborn et al. 2011).”
• HADRON–QUARK CROSSOVER AND MASSIVE HYBRID STARS WITH STRANGENESS (2012, background): “…such a heavy NS can have exotic components in the central core (Özel et al. (2010); Kurkela et al. (2010); Kim et al. (2011); Klahn et al. (2011); Lattimer et al. (2010); Weissenborn et al. (2011); Bonanno et al. (2012); Chen et al. (2012); Schramm et al. (2012); Whittenbury et al. (2012)).”