Astrophysical constraints on the confining models: The field correlator method

Baldo, M.; Burgio, G. F.; Castorina, P.; Plumari, Salvatore; Zappalà, Dario

doi:10.1103/physrevd.78.063009

Cited by 37 publications

(64 citation statements)

References 48 publications

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“…A similar study has been performed in Ref. [51], where a microscopic EOS derived with the BruecknerHartree-Fock approximation [52][53][54] has been employed to describe the hadronic phase, whereas, for the quark phase, the FCM has been used as in the present work. The properties of absolutely stable [23] strange quark matter and strange stars have been recently investigated within the FCM by the author of Ref.…”

Section: Introductionmentioning

confidence: 99%

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Quark deconfinement transition in neutron stars with the field correlator method

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Bombaci

2013

Phys. Rev. D

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A phase of strong interacting matter with deconfined quarks is expected in the core of massive neutron stars. In this article, we perform a study of the hadron-quark phase transition in cold (T = 0) neutron star matter and we calculate various structural properties of hybrid stars. For the quark phase, we make use of an equation of state (EOS) derived with the field correlator method (FCM) recently extended to the case of nonzero baryon density. For the hadronic phase, we consider both pure nucleonic and hyperonic matter, and we derive the corresponding EOS within a relativistic mean field approach. We make use of measured neutron star masses, and particularly the mass M = 1.97 ± 0.04 M of PSR J1614-2230 to constrain the values of the gluon condensate G2, which is one of the EOS parameters within the FCM. We find that the values of G2 extracted from the mass measurement of PSR J1614-2230 are consistent with the values of the same quantity derived within the FCM from recent lattice QCD calculations of the deconfinement transition temperature at zero baryon chemical potential. The FCM thus provides a powerful tool to link numerical calculations of QCD on a space-time lattice with measured neutron star masses. --------------------

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Section: Introductionmentioning

confidence: 99%

“…With the purpose to compare with previous studies [51], we also make use of the so-called Maxwell construction for the phase transition. In this case, one imposes that each phase in equilibrium is separately charge neutral.…”

Section: Phase Transition In Beta-stable Neutron Star Mattermentioning

confidence: 99%

Quark deconfinement transition in neutron stars with the field correlator method

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Bombaci

2013

Phys. Rev. D

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“…The FCM has been extended to finite temperature and chemical potential [17][18][19] and the analytical results, in the gaussian approximation, are in good agreement with the lattice data on thermodynamic quantities, (available for small µ B only). Moreover, the application of the FCM for large values of the chemical potential allows to obtain a simple expression of the Equation of State of the quark-gluon matter in the range of the baryon density relevant for the study of neutron stars [25,26,28]. magnetic field, B, has been included in the FCM equation of state [20,21] and the quark (q) pressure and the gluon (g) pressure turn out to be…”

Section: Field Correlator Methodsmentioning

confidence: 99%

QCD equation of state and cosmological parameters in the early universe

2015

Self Cite

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The time evolution of cosmological parameters in early Universe at the deconfinement transition is studied by an equation of state (EoS) which takes into account the finite baryon density and the background magnetic field. The non perturbative dynamics is described by the Field Correlator Method (FCM) which gives, with a small number of free parameters, a good fit of lattice data. The entire system has two components, i.e. the quark-gluon plasma and the electroweak sector, and the solutions of the Friedmann equation show that the scale factor, a(t), and H(t) = (1/a)da/dt are weakly dependent on the EoS, but the deceleration parameter, q(t), and the jerk, j(t), are strongly modified above the critical temperature T c , corresponding to a critical time t c ≃ 20 − 25µs. The time evolution of the cosmological parameters suggest that above and around T c there is a transient state of acceleration typical of a matter dominated Universe; this is entailed by the QCD strong interaction driven by the presence of massive colored objects.

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“…All our results have been obtained in terms of these two quantities considered as independent on density [25,26]. Recently in Ref.…”

Section: Equation Of State Of Neutron Star Mattermentioning

confidence: 99%

Hybrid neutron stars with the field correlator method

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Bombaci

2014

J. Phys.: Conf. Ser.

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Abstract. We study the quark deconfinement phase transition in cold (T = 0) neutron star matter and we calculate various structural properties of hybrid stars. For the quark phase, we use an equation of state (EOS) based on the Field Correlator Method (FCM) extended to the case of nonzero baryon density. For the confined hadronic phase we use a relativistic mean field model considering both pure nucleonic and hyperonic matter. We constrain the values of the gluon condensate G2, which is one of the EOS parameter within the FCM, making use of the measured mass, M = 1.97 ± 0.04 M , of the neutron star in PSR J1614-2230. Our results show that the values of G2 extracted from the mass measurement of PSR J1614-2230 are consistent with the values of the same quantity derived, within the FCM, from recent lattice QCD calculations of the deconfinement transition temperature at zero baryon chemical potential. IntroductionNeutron stars are the densest macroscopic objects in the universe. A large variety of calculations of neutron star structures [1, 2, 3, 4] predict a maximum stellar central density (the one for the maximum mass star configuration) in the range of 4 − 8 times the saturation density (∼ 2.8 × 10 14 g/cm 3 ) of nuclear matter. Therefore, neutron stars, can be viewed as natural laboratories to explore the low temperature T and high baryon chemical potential region of the phase diagram of quantum chromodynamics (QCD) [5,6]. Under these conditions nonperturbative aspects of QCD are expected to play an essential role, and a transition to a phase with deconfined quarks and gluon is expected to occur and to effect a number of interesting astrophysical phenomena [7,8,9,10,11,12,13,14,15].Current high-precision numerical calculations of QCD on a space-time lattice at zero baryon chemical potential μ b (zero baryon density) seem to indicate that at high temperature and for physical values of the quark masses, the transition to quark gluon plasma is a crossover [16] rather than a real phase transition.Unluckily, present lattice QCD calculations at finite baryon chemical potential are plagued with the so called "sign problem", which makes them unrealizable by all presently known lattice methods. Thus, in order to explore the QCD phase diagram at low temperature T and high μ b , it is necessary to adopt some approximations in QCD or to apply some QCD effective model.Along these lines the MIT bag model [17] and the Nambu Jona-Lasinio (NJL) model [18] have been widely used to calculate the quark matter EOS. However the MIT bag and the NJL

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Astrophysical constraints on the confining models: The field correlator method

Cited by 37 publications

References 48 publications

Quark deconfinement transition in neutron stars with the field correlator method

Quark deconfinement transition in neutron stars with the field correlator method

QCD equation of state and cosmological parameters in the early universe

Hybrid neutron stars with the field correlator method

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