Relativistic equations of state in a Thomas-Fermi approach for neutron stars

Espíndola, Aquino L.; Menezes, D. P.

doi:10.1103/physrevc.65.045803

Cited by 25 publications

(27 citation statements)

References 21 publications

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“…We use m u = m d = 5.5 MeV, m s = 150.0 MeV and Bag = (180 MeV) 4 . If m u , m d and m s are chosen as in the NJL model, the behavior of the properties of interest are not altered, since they are more dependent on the Bag pressure than on small differences in the quark masses.…”

Section: B the Mit Bag Modelmentioning

confidence: 99%

Quark stars within relativistic models

Menezes¹,

Providência²,

Melrose³

2006

J. Phys. G: Nucl. Part. Phys.

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Lately, it has been suggested that strange (quark) stars can be responsible for glitches and other observational features of pulsars. Some discussions on whether quark stars, if really exist, are bare or crusted are also a source of controversy in the recent literature. In the present work we use the Nambu-Jona-Lasinio model, known to incorporate chiral symmetry, necessarily present in the QCD formalism, in order to describe quark star properties. We compare our results for the stars and the features of the model with the much simpler model normally used in the description of strange stars, namely the MIT bag model. We also investigate the differences in the stellar properties which arise due to the presence of the crust. We show that the NJL model produces results which are somewhat different as compared with the MIT model. PACS number(s): 26.60.+c,24.10.Jv, 21.65.+f,95.30.Tg

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Section: B the Mit Bag Modelmentioning

confidence: 99%

Quark stars within relativistic models

Menezes¹,

Providência²,

Melrose³

2006

J. Phys. G: Nucl. Part. Phys.

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“…The composition of neutron stars remains a source of speculation. Three of the possibilities are that 1) the stars are formed by hadrons plus leptons (hadronic stars) [3], 2) they are formed by quarks plus leptons (strange or quark stars) [4] and 3) that they are hybrid, formed by hadrons plus leptons and quarks plus leptons, bearing [5] or nor a mixed phase [6].…”

Section: Introductionmentioning

confidence: 99%

Adiabatic index of hot and cold compact objects

Casali¹,

Menezes²

2010

Braz. J. Phys.

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In the present work we calculate the adiabatic index of neutron stars formed by hadronic or quarkionic matter, under two possible conditions, with and without trapped neutrinos, and for two values of the entropy per baryon S = 0, 2 k B / baryon. We use the nonlinear Walecka model to describe hadronic stars, and the MIT bag model to describe quark stars. Particle fractions for each case are obtained and the appearance of particles are compared with drops in the adiabatic index, whenever possible.

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“…The effect of many possible EOS has been studied in this context (Glendenning 2000;Prakash et al 1997). One class of EOS is based on the assumption that the neutron star is composed only of hadrons (Espíndola & Menezes 2002;Santos & Menezes 2004) plus an essential small admixture of electrons. In order to construct appropriate EOS for these hadronic stars, one must rely on models which describe nuclear matter's bulk properties.…”

Section: Introductionmentioning

confidence: 99%

Strange Star Equations of State Revisited

Menezes

Melrose

2005

Publ. – Astron. Soc. Aust

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Motivated by recent suggestions that strange stars can be responsible for glitches and other observational features of pulsars, we review some possible equations of state and their implications for models of neutron, hybrid, and strange stars. We consider the MIT bag model and also strange matter in the colourflavour locked phase. The central energy densities for strange stars are higher than the central densities of ordinary neutron stars. Strange stars are bound by the strong force and so can also rotate much faster than neutron stars. These results are only weakly dependent on the model used for the quark matter. If just one of the existing mass-to-radius ratio constraint is valid, most neutron stars equations of state are ruled out, but all the strange stars equations of state presented in this work remain consistent with the constraint.

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Relativistic equations of state in a Thomas-Fermi approach for neutron stars

Cited by 25 publications

References 21 publications

Quark stars within relativistic models

Quark stars within relativistic models

Adiabatic index of hot and cold compact objects

Strange Star Equations of State Revisited

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