Tidal deformability of quark stars with repulsive interactions

Albino, M. B.; Fariello, Ricardo; Navarra, F. S.

doi:10.1103/physrevd.104.083011

Cited by 16 publications

(19 citation statements)

References 73 publications

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“…In the present work, we use the modified NJL model to study both ud and uds quark matter and the corresponding self-bound stars. For this we need further extend the model [39] to include the vector interactions shown as necessary for the study of dense stellar matter and compact stars [14,[40][41][42][43][44][45][46][47][48]. This is also one of the first studies to evaluate systematically the stability of both strange and nonstrange quark matter, in connection with available multi-messenger stellar observations.…”

Section: Introductionmentioning

confidence: 99%

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Yuan,

Li,

Miao

et al. 2022

Preprint

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The stability and equation of state of quark matter are studied within both two-flavor and (2+1)-flavor Nambu-Jona-Lasinio (NJL) models including the vector interactions. With a free parameter α, the Lagrangian is constructed by two parts, the original NJL Lagrangian and the Fierz transformation of it, as L = (1 − α)LNJL + αLFierz. We find that there is a possibility for both ud nonstrange and uds strange matter being absolute stable, depending on the interplay of the confinement with quark vector interaction and the exchange interaction channels. The calculated quark star properties can reconcile with the recently measured masses and radii of PSR J0030+0451 and PSR J0740+6620, as well as the tidal deformability of GW170817. Furthermore, the more strongly-interacting quark matter in the nonstrange stars allows a stiffer equation of state and consequently a higher maximum mass (∼ 2.7 M ) than the strange ones (∼ 2.1 M ). The sound velocities in strange and nonstrange quark star matter are briefly discussed compared to those of neutron star matter.

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Section: Introductionmentioning

confidence: 99%

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Yuan,

Li,

Miao

et al. 2022

Preprint

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“…The LOVE-Q relation is universal for neutron stars and quark stars as shown by (Yagi & Yunes 2013). Consequently if the paritciapting stars in the binary mergers are treated to be SS, then also the bounds on Λ and Λ are applicable to constrain the SQM models (Li et al 2021;Lourenço et al 2021;Albino et al 2021). Based on the GW170817 event data as well as the respective electromagnetic counterparts, bounds on the maximum gravitational mass of the dense matter compact star is estimated as 𝑀 ≤ 2.2 M (Margalit & Metzger 2017;Shibata et al 2017;Rezzolla et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Compact star merger events with stars composed of interacting strange quark matter

Kumar,

Thapa,

Sinha

2022

Preprint

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We investigate the properties of stars participating in double compact star merger events considering interacting model of stable strange quark matter. We model the matter making it compatible with the recent astrophysical observations of compact star mass-radius and gravitational wave events. In this context we consider modified MIT bag model and vector bag model with and without self interaction. We find new upper bound on tidal deformability of 1.4 𝑀 strange star corresponding to the upper bound of effective tidal deformability inferred from gravitational wave event. Range of compactness of 1.4 𝑀 strange star is obtained as 0.175 ≤ 𝐶 1.4 ≤ 0.199. Radius range of 1.5𝑀 primary star is deduced to be 10.57 ≤ 𝑅 1.5 ≤ 12.04 km, following stringent GW170817 constraints. GW190425 constraints provide with upper limit on radius of 1.7 solar mass strange star that it should be less than 13.41 km.

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“…Até aqui, consideramos que as estrelas de nêutrons são constituídas inteiramente por matéria de quarks. Neste caso, elas são chamadas de estrelas de quarks [11,12,13,14,15]. Entretanto, não há um consenso em relação a fase em que a matéria se apresenta no interior das estrelas de nêutrons.…”

Section: Estrelas De Nêutronsunclassified

“…Em seguida vamos compará-los com os dados observacionais e verificar se a MFTQCD satisfaz as novas restrições impostas pelas observações. Esta primeira parte do trabalho resultou no artigo publicado em [11]. Em seguida, nos dedicamos ao estudo de estrelas híbridas.…”

Section: Objetivos Deste Trabalhounclassified

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Natureza da transição de fase quark-hádron e consequências para a estrutura estelar

Albino¹

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Neutron stars are the second most dense objects in the universe (only less dense than black holes) and have a relatively low temperature. Because of these features, neutron star matter lies in a poorly understood region of the QCD phase diagram. Neutron stars can work as laboratories for the study of cold and dense matter.In this work, we used the MFTQCD (Mean-Field Theory of Quantum Chromodynamics) and we obtained the mass-radius diagram and the tidal deformability. Comparing these results with the experimental data, we conclude that the MFTQCD remains a good model to describe the properties of neutron stars; however, the parameter window is now narrower. Next, we studied the impact of the nature of the phase transition on neutron star properties. We used an equation of state which combines hadronic matter and quark matter. We control the smoothness of the quark-hadron transition by varying the free parameter ρ c . Our results indicate that a sharp phase transition is more compatible with experimental data.

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Tidal deformability of quark stars with repulsive interactions

Cited by 16 publications

References 73 publications

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Interacting $ud$ and $uds$ quark matter at finite densities and quark stars

Compact star merger events with stars composed of interacting strange quark matter

Natureza da transição de fase quark-hádron e consequências para a estrutura estelar

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