Twin stars within the SU(3) chiral quark-meson model

Zacchi, Andreas; Tolós, Laura; Schaffner-Bielich, J.

doi:10.1103/physrevd.95.103008

Cited by 42 publications

(37 citation statements)

References 30 publications

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“…Twin star solutions could not be found due to the abrupt decrease of the speed of sound c 2 s at the phase transition contrary to the abrupt increase modeled here. It is in-teresting to note that in [31] twin star solutions resulting from a SU(3) quark matter EoS only, with a chiral-like crossover phase transition, were found. Heiniman et.…”

Section: Discussionmentioning

confidence: 99%

“…Depending on the features of the transition between the inner and outer parts of hybrid stars, a so called twin star configuration might arise, i.e. a third family of compact stars appears with alike masses as the second family branch of normal neutron or strange quark stars [21][22][23][24][25][26][27][28][29][30][31]. With space missions such as NICER (Neutron star Interior Composition ExploreR) [32], high-precision X-ray astronomy will be able to offer precise measurements of masses and radii of compact stars [33].…”

Section: Introductionmentioning

confidence: 99%

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Classifications of twin star solutions for a constant speed of sound parameterized equation of state

2018

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We explore the possible mass radius relation of compact stars for the equation of states with a first order phase transition. The low density matter is described by a nuclear matter equation of state resulting from fits to nuclear properties. A constant speed of sound parametrization is used to describe the high density matter phase with the speed of sound c 2 s = 1. A classification scheme of four distinct categories including twin star solutions, i. e. solutions with the same mass but differing radii, is found which are compatible with the M ≥ 2M pulsar mass constraint. We show the dependence of the mass and radius differences on the transition parameters and delineate that higher twin star masses are more likely to be accompanied by large radius differences. These massive twin stars are generated by high values of the discontinuity in the energy density and the lowest possible values of the transition pressure that still result in masses of M ≥ 2M at the maximum of the hadronic branch. arXiv:1707.07524v1 [astro-ph.HE]

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

2018

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“…Taking a density dependent hadronic EoS and a density dependent chiral quark matter EoS, the transition between the two phases was studied and conditions for the appearance of twin stars were discused. This work was further extended [48,49] to finding a new stable solutions of the Tolman-Oppenheimer-Volkoff equations for quark stars. These new solutions were found to exhibit two stable branches in the mass-radius relation, allowing for twin stars; i.e., two stable quark star solutions with the same mass, but distinctly different radii.…”

Section: The Fock Termmentioning

confidence: 90%

Quark–Meson-Coupling (QMC) model for finite nuclei, nuclear matter and beyond

Guichon

Stone

Thomas

2018

Progress in Particle and Nuclear Physics

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The Quark-Meson-Coupling model, which self-consistently relates the dynamics of the internal quark structure of a hadron to the relativistic mean fields arising in nuclear matter, provides a natural explanation to many open questions in low energy nuclear physics, including the origin of many-body nuclear forces and their saturation, the spin-orbit interaction and properties of hadronic matter at a wide range of densities up to those occurring in the cores of neutron stars.Here we focus on four aspects of the model (i) a full comprehensive survey of the theory, including the latest developments, (ii) extensive application of the model to ground state properties of finite nuclei and hypernuclei, with a discussion of similarities and differences between the QMC and Skyrme energy density functionals, (iii) equilibrium conditions and composition of hadronic matter in cold and warm neutron stars and their comparison with the outcome of relativistic mean-field theories and, (iv) tests of the fundamental idea that hadron structure changes in-medium.

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“…A first order chiral phase transition yielding twin stars as in the MFA, see e.g. [18], was not found in the eMFA. Compared to the mean field case, the EoSs show a smooth behaviour due to the additional term in the potential coming from the fermion vacuum term.…”

Section: Discussionmentioning

confidence: 86%

“…Rearranging the entries of eq. (3) gives 18) and the transformation from the physical nonstrangestrange basis to the mathematical basis reads…”

Section: A Renormalized Vacuum Parameters Of the Su(3) Quark Meson Mmentioning

confidence: 99%

Implications of the fermion vacuum term in the extended SU(3) quark meson model on compact star properties

Zacchi¹,

Schaffner-Bielich²

2019

Phys. Rev. D

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We study the impact of the fermion vacuum term in the SU(3) quark meson model on the equation of state and determine the vacuum parameters for various sigma meson masses. We examine its influence on the equation of state and on the resulting mass radius relations for compact stars. The tidal deformability Λ of the stars is studied and compared to the results of the mean field approximation. Parameter sets which fulfill the tidal deformability bounds of GW170817 together with the observed two solar mass limit turn out to be restricted to a quite small parameter range in the mean field approximation. The extended version of the model does not yield solutions fulfilling both constraints. Furthermore, no first order chiral phase transition is found in the extended version of the model, not allowing for the twin star solutions found in the mean field approximation.

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Twin stars within the SU(3) chiral quark-meson model

Cited by 42 publications

References 30 publications

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

Classifications of twin star solutions for a constant speed of sound parameterized equation of state

Quark–Meson-Coupling (QMC) model for finite nuclei, nuclear matter and beyond

Implications of the fermion vacuum term in the extended SU(3) quark meson model on compact star properties

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