Nuclear Matter Mean Field with Extended NJL Model

Providência, C.; Moreira, J. António; Providência, João da; Moszkowski, S. A.

doi:10.1063/1.1570575

Cited by 3 publications

(4 citation statements)

References 18 publications

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“…However, as the chiral symmetry is important in strong interactions, it is relevant to introduce it for DM. Similar to baryons [51][52][53][54][55][56][57][58][59][60], the Lagrangian density for self-interacting fermionic DM with chiral symmetry (DMC) is given as follows:…”

Section: B Dark Mattermentioning

confidence: 99%

“…The spontaneous breaking of chiral symmetry is very important in strong interactions. Therefore, the NJL model is widely used on the nucleonic level [51][52][53][54][55][56][57][58][59][60] and on the quark level [61][62][63][64][65][66][67][68][69][70]. For quarks, since the NJL model neglects the gluon degrees of freedom, it does not confine the quarks.…”

mentioning

confidence: 99%

“…Similar to the non-linear model, this problem has been solved by introducing a scalar-vector interaction in the NJL model [51]. Since then, the NJL model on the nucleonic level has been widely employed in investigating properties of NSs and nuclei [52][53][54][55][56][57][58][59][60].…”

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confidence: 99%

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Dark matter with chiral symmetry admixed with hadronic matterin compact stars *

Wei¹,

Feng²

2022

Chinese Phys. C

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With the two-fluid TOV equation, the properties of dark matter (DM) admixed NSs (DANSs) have been studied. Different from previous studies, we found that increase of the maximum mass and decrease of the radius of 1.4 $M_\odot$ can occur simultaneously in DANS. This stems from the fact that the equation of state (EOS) of DM can be very soft at low density but very stiff at high density. It is well known that the IU-FSU and XS models can not reproduce the neutron star (NS) with a maximum mass greater than 2.0 $M_\odot$. However, considering IU-FSU and XS models in DANS, there are always mass and interactions of DM that can reproduce a maximum mass greater than 2.0 $M_\odot$ and the radius of 1.4 $M_\odot$ below 13.7km. The difference of DANS between the DM with chiral symmetry (DMC) and the DM with meson exchange (DMM) becomes obvious when the central energy density ratio of the DM is greater than one of the NM. When the central energy density ratio of the DM is greater than one of the NM, the DMC model with the DM mass of 1000 MeV still can reproduce a maximum mass greater than 2.0 $M_\odot$ and the radius of 1.4 $M_\odot$ below 13.7km. In the same case, although the maximum mass of DANS with the DMM model is greater than 2.0 $M_\odot$ , the radius of 1.4 $M_\odot$ with the DMM model will surpass 13.7km obviously. \com{In two-fluid system, it is worth noting that the maximum mass of DANS can be larger than 3.0 $M_\odot$. As a consequence, the dimensionless tidal deformability $\Lambda_{CP}$ of DANS with 1.4 $M_\odot$, which increase with increasing the maximum mass of DANS, could be larger than 800 when the radius of DANS with 1.4 $M_\odot$ is about 13.0km.}

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Section: B Dark Mattermentioning

confidence: 99%

mentioning

confidence: 99%

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Dark matter with chiral symmetry admixed with hadronic matterin compact stars *

Wei¹,

Feng²

2022

Chinese Phys. C

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“…In [18] and [21], the hadron-quark phase transition was investigated with the help of two different models, namely, the non-linear Walecka model (NLWM) for the hadronic phase and the MIT bag model for the quark phase. A formalism we understand as a more adequate one was used in [19,26,27] at zero temperature and by [20] for finite temperatures, all considering NJL-type models for the two phases. To describe the hadron phase, the standard NJL model with vector interaction is extended to include a scalar-vector channel in order to render the model capable of saturation at low densities [28].…”

Section: Introductionmentioning

confidence: 99%

Hadron-quark phase transition: the QCD phase diagram and stellar conversion

Graeff

Alloy²,

Marquez³

et al. 2019

J. Cosmol. Astropart. Phys.

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Different extensions of the Nambu-Jona-Lasinio model, known to satisfy expected QCD chiral symmetry aspects, are used to investigate a possible hadron-quark phase transition at zero temperature and to build the corresponding binodal sections. We have shown that the transition point is very sensitive to the model parameters and that both pressure and chemical potential increase drastically with the increase of the vector interaction strength in the quark sector. Within the same framework, the possibility of quark and hybrid star formation is analyzed. The same conclusions drawn before with respect to the coexistence pressure and chemical potentials are reinforced. We conclude that even if a transition from a metastable hadronic star to a quark star is thermodinamically possible, it is either energetically forbidden or gives rise to a blackhole. Nevertheless, conversions from metastable to hybrid stars are possible, but the mass difference between both compact objects is very small, never larger than 0.2 M ⊙ .

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Symmetry energy and neutron star properties in the saturated Nambu–Jona-Lasinio model

et al. 2016

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Considering the importance of Lorentz invariance and chiral symmetry, we adopt the Nambu-Jona-Lasinio (NJL) model that ensures the nuclear matter saturation properties to study the density dependence of the symmetry energy. The negative symmetry energy at high densities that is usually dubbed the super-soft symmetry energy can be obtained from introducing a chiral isovector-vector interaction in the lagrangian, but should be ruled out by the neutron star (NS) stability in the mean-field approximation. It is found that the isovector-scalar interaction in the NJL model can play an important role in softening of the symmetry energy. We have investigated NS properties. The NS maximum mass obtained with various isovector-scalar couplings and momentum cutoffs is well above the 2M⊙, and the NS radius obtained well meets the limits extracted from recent measurements. In particular, the significant reduction of the canonical NS radius occurs with the moderate decrease of the slope of the symmetry energy, while the effect of the symmetry energy on the NS maximum mass remains insignificant as usual.

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Nuclear Matter Mean Field with Extended NJL Model

Cited by 3 publications

References 18 publications

Dark matter with chiral symmetry admixed with hadronic matterin compact stars *

Dark matter with chiral symmetry admixed with hadronic matterin compact stars *

Hadron-quark phase transition: the QCD phase diagram and stellar conversion

Symmetry energy and neutron star properties in the saturated Nambu–Jona-Lasinio model

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