Self-bound interacting QCD matter in compact stars

Franzon, B.; Fogaça, D. A.; Navarra, F. S.; Horvath, J. E.

doi:10.1103/physrevd.86.065031

Cited by 27 publications

(50 citation statements)

References 26 publications

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“…The model presented below was proposed in [24] and it was applied to study the cold and dense quark gluon plasma in the inner core of neutron stars [25]. In [24] we start from the QCD Lagrangian and split the gluon field into low and high momentum modes.…”

Section: Modelmentioning

confidence: 99%

The quark gluon plasma equation of state and the expansion of the early Universe

2015

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Our knowledge of the equation of state of the quark gluon plasma has been continuously growing due to the experimental results from heavy ion collisions, due to recent astrophysical measurements and also due to the advances in lattice QCD calculations. The new findings about this state may have consequences on the time evolution of the early Universe, which can estimated by solving the Friedmann equations. The solutions of these equations give the time evolution of the energy density and also of the temperature in the beginning of the Universe. In this work we compute the time evolution of the QGP in the early Universe, comparing several equations of state, some of them based on the MIT bag model (and on its variants) and some of them based on lattice QCD calculations. Among other things, we investigate the effects of a finite baryon chemical potential in the evolution of the early Universe.

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Section: Modelmentioning

confidence: 99%

The quark gluon plasma equation of state and the expansion of the early Universe

2015

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“…This model was proposed in [12] to study the cold and dense quark gluon plasma in the inner core of neutron stars [13]. It is derived from the QCD Lagrangian treated in the mean field approximation.…”

Section: Modelmentioning

confidence: 99%

The time evolution of the quark gluon plasma in the early Universe

Sanches

Fogaça²,

Navarra³

2015

J. Phys.: Conf. Ser.

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Abstract.Our knowledge of the equation of state of the quark gluon plasma has been continuously growing due to the experimental results from heavy ion collisions and also due to the advances in lattice QCD calculations. The new findings about this state may have consequences on the time evolution of the early Universe, which can estimated by solving the Friedmann equations. The solutions of these equations give the time evolution of the energy density and also of the temperature in the beginning of the Universe. In this work we compute the time evolution of the QGP in the early Universe, comparing several equations of state, some of them based on the MIT bag model (and on its variants) and some of them based on lattice QCD calculations. Among other things, we investigate the effects of a finite baryon chemical potential in the evolution of the early Universe. IntroductionIn the last ten years relativistic heavy-ion collision experiments have provided us with information about the properties of matter in the early Universe (at the time when its age was about 10 microseconds and its temperature was higher than 150 MeV). It is believed that, during this period, the Universe was formed by a hot phase of deconfined quarks and gluons, i.e., a quark gluon plasma (QGP). In parallel with these experimental developments there has been a significant progress on the theoretical side, coming from the numerical simulation of finite temperature QCD on a lattice. The new findings about the nature of the QGP motivate us to investigate their consequences in the primordial Universe. This can be done by solving the Friedmann equations, which allow us to determine the precise time evolution of the thermodynamic quantities in the early Universe.Previous works along this line and with the same motivation already exist in the literature. For a review see, e.g., [1] and for recent papers on the subject see [2,3] and references therein. Most of these works focused on the nature of the phase transiton from the QGP to the hadron gas. There are exotic phenomena associated with the order of the phase transition. In [3] a realistic EOS was used in cosmological calculations. In this EOS the transition was actually a crossover and not a first order transition as commonly believed until recent years. The results showed a very smooth time dependence of various thermodynamic quantities and suggested indirectly that there are small chances for the observation of various exotic phenomena such as quark nuggets, strangelets, cold dark matter clumps, etc. Such phenomena are associated typically with first order phase transitions. Apart from these exotic phenomena, changing the

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“…In [2] we presented the derivation of the equation of state starting from the QCD Lagrangian density. To proceed to the stellar conditions, we consider the EOS from [3] which is an improvement of the EOS obtained in [2] with quarks u, d, s and also electrons in chemical equilibrium maintained by the weak processes. The neutrinos are assumed to escape and do not contribute to the pressure and energy density.…”

Section: Equation Of Statementioning

confidence: 99%