Finite size effects on kaonic “pasta” structures

Maruyama, Toshiki; Tatsumi, Toshitaka; Voskresensky, D. N.; Tanigawa, Tomonori; Endo, Tomoki; Chiba, Satoshi

doi:10.1103/physrevc.73.035802

Cited by 76 publications

(84 citation statements)

References 79 publications

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“…Since the matter in the core of neutron stars is possibly compressed to several times of the saturation nuclear density, new particles and even hadron-quark phase transitions may appear in the interior of these compact objects [1][2][3][4][5][6][7][8][9][10][11][12][13]. On the other hand, the EoS of neutron star matter is crucial for the macroscopic features of neutron stars.…”

Section: Introductionmentioning

confidence: 99%

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

et al. 2013

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The hadron-quark phase transition in the core of massive neutron stars is studied with a newly constructed two-phase model. For nuclear matter, a nonlinear Walecka type model with general nucleon-meson and meson-meson couplings, recently calibrated by Steiner, Hemper and Fischer, is taken. For quark matter, a modified Polyakov-Nambu-Jona-Lasinio (mPNJL) model, which gives consistent results with lattice QCD data, is used. Most importantly, we introduce an isoscalar-vector interaction in the description of quark matter, and we study its influence on the hadron-quark phase transition in the interior of massive neutron stars. With the constraints of neutron star observations, our calculation shows that the isoscalar-vector interaction between quarks is indispensable if massive hybrids star exist in the universe, and its strength determines the onset density of quark matter, as well as the mass-radius relations of hybrid stars. Furthermore, as a connection with heavy-ioncollision experiments we give some discussions about the strength of isoscalar-vector interaction and its effect on the signals of hadron-quark phase transition in heavy-ion collisions, in the energy range of the NICA at JINR-Dubna and FAIR at GSI-Darmstadt facilities.

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Section: Introductionmentioning

confidence: 99%

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

et al. 2013

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“…To clarify charge-screening effects, we also perform calculations without including screening [9,14,15]. We also adopt the EOS derived in a previous paper [9] and then apply it to the TOV equation [10,16].…”

Section: Formalism and Numerical Resultsmentioning

confidence: 99%

Impact of Rotation on Quark–Hadron Hybrid Stars

Endo

2018

Proceedings of the Workshop on Quarks and Compact Stars 2017 (QCS2017)

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Many recent observations give restrictions to the equation of state (EOS) for high-density matter. Theoretical studies are needed to try to elucidate these EOSs at high density and/or temperature. With the many known rapidly rotating neutron stars, e.g., pulsars, several theoretical studies have tried to take into account the effects of rotation. In our study of these systems, we find that one of our EOSs is consistent with recent observation, whereas the other is inconsistent.

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“…Namely, whether nonuniform (pasta) structures appear in the HQ mixed phase is subject to a balance between the surface tension and the Coulomb repulsion [44,48], which is similar to the situation in the crust [38] and kaon condensed matter [49]. However, to determine the surface tension with the experiments on the Earth is quite difficult because temperature becomes too high for the HQ mixed phase to appear during the relativistic heavy-ion collisions.…”

Section: Introductionmentioning

confidence: 99%

Shear oscillations in the hadron–quark mixed phase

2013

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Inside neutron stars, the hadron-quark mixed phase is expected during the first order phase transition from the hadron phase to the quark phase. The geometrical structure of the mixed phase strongly depends on the surface tension at the hadron-quark interface. We evaluate the shear modulus which is one of the specific properties of the hadron-quark mixed phase. As an application, we study shear oscillations due to the hadron-quark mixed phase in neutron stars. We find that the frequencies of shear oscillations depend strongly on the surface tension; with a fixed stellar mass, the fundamental frequencies are almost proportional to the surface tension. Thus, one can estimate the value of surface tension via the observation of stellar oscillations with the help of the information on the stellar mass.

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Finite size effects on kaonic “pasta” structures

Cited by 76 publications

References 79 publications

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

Impact of Rotation on Quark–Hadron Hybrid Stars

Shear oscillations in the hadron–quark mixed phase

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