Quark matter nucleation in hot hadronic matter

Bombaci, Ignazio; Logoteta, Domenico; Panda, P. K.; Providência, Constança; Vidaña, Isaac

doi:10.1016/j.physletb.2009.09.039

Cited by 78 publications

(123 citation statements)

References 48 publications

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“…As emphasized in earlier works [4][5][6][7][8][9][10][11], an important characteristic of the deconfinement transition in neutron stars, is that just deconfined quark matter is transitorily out of equilibrium with respect to weak interactions. In fact, depending on the temperature, the transition should begin with the quantum or thermal nucleation of a small quarkmatter drop near the center of the star.…”

Section: Introductionmentioning

confidence: 86%

Deconfinement transition in protoneutron stars: Analysis within the Nambu–Jona-Lasinio model

et al. 2010

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We study the effect of color superconductivity and neutrino trapping on the deconfinement transition of hadronic matter into quark matter in a protoneutron star. To describe the strongly interacting matter a two-phase picture is adopted. For the hadronic phase we use different parameterizations of a non-linear Walecka model which includes the whole baryon octet. For the quark matter phase we use an SU (3) f Nambu-Jona-Lasinio effective model which includes color superconductivity. We impose color and flavor conservation during the transition in such a way that just deconfined quark matter is transitorily out of equilibrium with respect to weak interactions. We find that deconfinement is more difficult for small neutrino content and it is easier for lower temperatures although these effects are not too large. In addition they will tend to cancel each other as the protoneutron star cools and deleptonizes, resulting a transition density that is roughly constant along the evolution of the protoneutron star. According to these results the deconfinement transition is favored after substantial cooling and contraction of the protoneutron star.

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Section: Introductionmentioning

confidence: 86%

Deconfinement transition in protoneutron stars: Analysis within the Nambu–Jona-Lasinio model

et al. 2010

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“…Under such conditions, a deconfinement transition to quark matter is possible and a hybrid star or a strange quark star can be formed. The conversion of the star is expected to start with the nucleation of small quark matter drops [7][8][9][10] which subsequently grow at the expenses of the gravitational energy extracted from the contraction of the object and/or through a strongly exothermic combustion process. Quark matter droplets with a variety of geometrical forms can also arise within the mixed hadron-quark phase that is expected to form inside hybrid stars if global charge neutrality is allowed [11].…”

Section: Introductionmentioning

confidence: 99%

Surface tension of highly magnetized degenerate quark matter

Lugones

Grunfeld

2017

Phys. Rev. C

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We study the surface tension of highly magnetized three flavor quark matter within the formalism of multiple reflection expansion (MRE). Quark matter is described as a mixture of free Fermi gases composed by quarks u, d, s and electrons, in chemical equilibrium under weak interactions. Due to the presence of strong magnetic fields the particles' transverse motion is quantized into Landau levels, and the surface tension has a different value in the parallel and transverse directions with respect to the magnetic field. We calculate the transverse and longitudinal surface tension for different values of the magnetic field and for quark matter drops with different sizes, from a few fm to the bulk limit. For baryon number densities between 2 − 10 times the nuclear saturation density, the surface tension falls in the range 2 − 20 MeV /fm 2 . The largest contribution comes from strange quarks which have a surface tension an order of magnitude larger than the one for u or d quarks and more than two orders of magnitude larger than for electrons. Our results show that the total surface tension is quite insensitive to the size of the drop. We also find that the surface tensions in the transverse and parallel directions are almost unaffected by the magnetic field if eB is below ∼ 5 × 10 −3 GeV 2 . Nevertheless, for higher values of eB, there is a significant increase in the parallel surface tension and a significant decrease in the transverse one with respect to the unmagnetized case.

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“…Thus these 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][7][8]. In this regime nonperturbative aspects of QCD are expected to play a crucial role, and a transition to a phase with deconfined quarks and gluons is expected to occur and to influence a number of interesting astrophysical phenomena [9][10][11][12][13][14][15][16].…”

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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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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Quark matter nucleation in hot hadronic matter

Cited by 78 publications

References 48 publications

Deconfinement transition in protoneutron stars: Analysis within the Nambu–Jona-Lasinio model

Deconfinement transition in protoneutron stars: Analysis within the Nambu–Jona-Lasinio model

Surface tension of highly magnetized degenerate quark matter

Quark deconfinement transition in neutron stars with the field correlator method

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