SQM studied in the Field Correlator Method

Pereira, Flávio

doi:10.1016/j.nuclphysa.2012.11.008

Cited by 9 publications

(13 citation statements)

References 48 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…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

View full text Add to dashboard Cite

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.

show abstract

Section: Confinementmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

View full text Add to dashboard Cite

show abstract

“…Recent studies about the strange quark matter hypothesis in the framework of the FCM (Pereira 2013), show that for some choices of the parameters G 2 and V 1 , the energy per baryon can be lower than the energy per nucleon of the 56 Fe. According to Pereira (2013), the stability window strongly depends on the values of the FCM parameters: as V 1 increases, from V 1 = 0 GeV to V 1 = 0.5 GeV, G 2 must decrease in order to keep the energy per baryon of the quark matter less than 930 MeV.…”

Section: Stability Of Quark Mattermentioning

confidence: 99%

“…According to Pereira (2013), the stability window strongly depends on the values of the FCM parameters: as V 1 increases, from V 1 = 0 GeV to V 1 = 0.5 GeV, G 2 must decrease in order to keep the energy per baryon of the quark matter less than 930 MeV.…”

Section: Stability Of Quark Mattermentioning

confidence: 99%

Constant entropy hybrid stars: a first approximation of cooling evolution

Mariani

Orsaria

Vucetich³

2017

A&A

View full text Add to dashboard Cite

Aims. We aim to study the possibility of a hadron-quark phase transition in the interior of neutron stars, taking into account different schematic evolutionary stages at finite temperature. We also discuss the strange quark matter stability in the quark matter phase.Furthermore, we aim to analyze the astrophysical properties of hot and cold hybrid stars, considering the constraint on maximum mass given by the pulsars J1614-2230 and J0348+0432. Methods. We have developed a computational code to construct semi-analytical hybrid equations of state at fixed entropy per baryon and to obtain different families of hybrid stars. An analytical approximation of the Field Correlator Method is developed for the quark matter equation of state. For the hadronic equation of state we use a table based on the relativistic mean field theory, without hyperons. The phase transition was obtained imposing the Maxwell conditions, by assuming a high surface tension at the interface hadron-quark. We solved the relativistic structure equations of hydrostatic equilibrium and mass conservation for hybrid star configurations. Results. For the different equations of state obtained, we calculated the stability window for the strange quark matter, lepton abundances, temperature profiles and contours profiles for the maximum mass star depending on the parameters of the Field Correlator Method. We also computed the mass-radius and gravitational mass-baryonic mass relationships for different hybrid star families. Conclusions. We have analyzed different stages of hot hybrid stars as a first approximation of the cooling evolution of neutron stars with quark matter cores. We obtain cold hybrid stars with maximum masses ≥ 2M for different combinations of the Field Correlator Method parameters. In addition, our study based on the gravitational mass -baryonic mass plane shows a late phase transition between hadronic and quark matter during the proto-hybrid star evolution, in contrast with previous studies of proto-neutron stars.

show abstract

“…In previous works, we outlined the main features of the FCM and showed the equations used to investigate strange stars and strange quark matter properties [38,39]. So, we now write only the main equations we need here.…”

Section: The Npeos At Zero Temperaturementioning

confidence: 99%

“…Recently we applied the FCM to investigate the properties of the strange stars and the SQM stability in Refs. [38,39]. Of particular significance is the gradual decrease of the widths of the SQM stability windows with the increase of V 1 , being zero at V 1 = 0.5 GeV , the value of V 1 determined from lattice calculations [40].…”

mentioning

confidence: 99%

On the anomalous mass defect of strange stars in the Field Correlator Method

Pereira

2016

Nuclear Physics A

Self Cite

View full text Add to dashboard Cite

We investigate general aspects of the mass defects of strange stars in the context of the Field Correlator Method, without magnetic field. The main parameters of the model that enter the corresponding nonperturbative equation of state of the quark gluon plasma are the gluon condensate G 2 and the large distance static QQ potential V 1 .We calculate mass defects of stellar configurations in the central density range 11 < log ρ c < 18. In general, the mass defects are strongly dependent on the model parameters. For a large range of values of G 2 and V 1 , we obtain anomalous mass defects with magnitudes around 10 53 erg , of the same order of the observed energies of gamma-ray bursts and neutrino emissions in SN1987A, and of the theoretically predicted energies of the quark-novae explosions.

show abstract

SQM studied in the Field Correlator Method

Cited by 9 publications

References 48 publications

Phases of Dense Matter in Compact Stars

Phases of Dense Matter in Compact Stars

Constant entropy hybrid stars: a first approximation of cooling evolution

On the anomalous mass defect of strange stars in the Field Correlator Method

Contact Info

Product

Resources

About