Strange stars properties calculated in the framework of the Field Correlator Method

Pereira, Flávio

doi:10.1016/j.nuclphysa.2011.05.004

Cited by 8 publications

(5 citation statements)

References 32 publications

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“…This feature is partially supported by lattice simulations at small chemical potential [43,60]. In the present work, the value of V 1 at T = 0 has been considered as a model parameter [51,55].…”

Section: Eos Of the Quark Phasementioning

confidence: 53%

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Quark deconfinement transition in neutron stars with the field correlator method

Logoteta

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: Eos Of the Quark Phasementioning

confidence: 53%

“…The properties of absolutely stable [23] strange quark matter and strange stars have been recently investigated within the FCM by the author of Ref. [55].…”

Section: Introductionmentioning

confidence: 99%

Quark deconfinement transition in neutron stars with the field correlator method

Logoteta

Bombaci

2013

Phys. Rev. D

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“…This model has the strength that at finite temperatures its input parameters (gluon con-densate G 2 and vector field V I ) can be fixed with lattice QCD. However, when these values are used for the construction of hybrid stars there is a problem to fulfill the 2 M constraint [325]. Moreover, no absolutely stable strange quark matter is obtained [326].…”

Section: Confinementmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are unique cosmic laboratories for probing the properties of matter under extreme conditions that cannot be reproduced in terrestrial laboratories. The interior of a neutron star, endowed with the highest magnetic fields known and with densities spanning about ten orders of magnitude from the surface to the centre, is predicted to exhibit various phases of dense strongly interacting matter, whose physics is reviewed in this chapter. The outer layers of a neutron star consist of a solid nuclear crust, permeated by a neutron ocean in its densest region, possibly on top of a nuclear "pasta" mantle. The properties of these layers and of the homogeneous isospin asymmetric nuclear matter beneath constituting the outer core may still be constrained by terrestrial experiments. The inner core of highly degenerate, strongly interacting matter poses a few puzzles and questions which are reviewed here together with perspectives for their resolution. Consequences of the dense-matter phases for observables such the neutron-star mass-radius relationship and the prospects to uncover their structure with modern observational programmes are touched upon.

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“…Recently the FC method was successfully applied to the study of phase transition in neutron stars [50,51] without m.f. and in the case of strange quarks and strange matter in [52]. It is interesting to investigate the role of m.f.…”

Section: Introductionmentioning

confidence: 99%

Quark-hadron thermodynamics in a magnetic field

Orlovsky

Simonov

2014

Phys. Rev. D

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Nonperturbative treatment of quark-hadron transition at nonzero temperature T and chemical potential µ in the framework of Field Correlator Method is generalized to the case of nonzero magnetic field B. A compact form of the quark pressure for arbitrary B, µ, T is derived. As a result the transition temperature is found as a function of B and µ, which depends on only parameters: vacuum gluonic condensate G 2 and the field correlator D E 1 (x), which defines the Polyakov loops and it is known both analytically and on the lattice. A moderate (25%) decrease of T c (µ = 0) for eB changing from zero to 1 GeV 2 is found. A sequence of transition curves in the (µ, T ) plane is obtained for B in the same interval, monotonically decreasing in scale for growing B.

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Strange stars properties calculated in the framework of the Field Correlator Method

Cited by 8 publications

References 32 publications

Quark deconfinement transition in neutron stars with the field correlator method

Quark deconfinement transition in neutron stars with the field correlator method

Phases of Dense Matter in Compact Stars

Quark-hadron thermodynamics in a magnetic field

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