Sexaquark dilemma in neutron stars and its solution by quark deconfinement

Shahrbaf, Mahboubeh; Blaschke, D.; Typel, S.; Farrar, Glennys R.; Alvarez-Castillo, David

doi:10.1103/physrevd.105.103005

Cited by 24 publications

(18 citation statements)

References 74 publications

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“…Those values correspond to the condensation of sexaquark exactly at saturation density and are in agreement with the results obtained in [6]. More details could be found in [20].…”

Section: Csqcd-ix-2022supporting

confidence: 91%

“…Considering the value of mass and the slope of the mass shift of sexaquark (m S , x), a detailed analysis within our model has been performed which shows the lower boundary is (1885, 0.03) [20]. Those values correspond to the condensation of sexaquark exactly at saturation density and are in agreement with the results obtained in [6].…”

Section: Csqcd-ix-2022supporting

confidence: 85%

“…The way the reasonable values for x have been derived is explained in [20]. The pressure as a function of baryon density is depicted in the left panel of Fig.…”

Section: Sexaquark Dilemma In Purely Hadronic Starsmentioning

confidence: 99%

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Appearance of sexaquark in the core of neutron stars as a candidate of dark matter

Shahrbaf

2023

J. Phys.: Conf. Ser.

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We study the appearance of sexaquark (uuddss) as a candidate of dark matter in the core of neutron stars while there has been no experimental evidence of this particle in laboratories so far. Regarding the observational constraints of supermassive pulsars as well as gravitational waves, we encounter a sexaquark dilemma for which we introduce a solution by quark deconfinement fulfilling all present constraints from multi-messenger astronomy, i.e., tidal deformability in accordance with GW170817 and maximum mass above the lower limit from PSR J0740+6620.

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“…Those values correspond to the condensation of sexaquark exactly at saturation density and are in agreement with the results obtained in [6]. More details could be found in [20].…”

Section: Csqcd-ix-2022supporting

confidence: 91%

Section: Csqcd-ix-2022supporting

confidence: 85%

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Appearance of sexaquark in the core of neutron stars as a candidate of dark matter

Shahrbaf

2023

J. Phys.: Conf. Ser.

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“…The hybrid quark-hadron EoS is obtained by matching the quark and hadron ones by means of the Maxwell construction corresponding to a first order phase transition. For the hadron part we use the DD2npY -T EoS [24], which agrees with the low density constraint from the chiral effective field theory [16] and includes nucleonic and hyperonic degrees of freedom. Fig.…”

Section: Relativistic Density Functional For Quark Mattermentioning

confidence: 99%

Early deconfinement of asymptotically conformal color-superconducting quark matter in neutron stars

Ivanytskyi

Blaschke²,

Fischer³

et al. 2022

EPJ Web Conf.

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We present a relativistic density functional approach to color superconducting quark matter that mimics quark confinement by a fast growth of the quasiparticle selfenergy in the confining region. The approach is shown to be equivalent to a chiral model of quark matter with medium dependent couplings. While the (pseudo)scalar sector of the model is fitted to the vacuum phenomenology of quantum chromodynamics, the strength of interaction in the vector and diquark channels is varied in order to provide the best agreement with the observational constraints on the mass-radius relation and tidal deformability of neutron stars modelled with our approach. In order to recover the conformal behavior of quark matter at asymptotically high densities we introduce a medium dependence of the vector and diquark couplings motivated by the non-perturbative gluon exchange. Our analysis signals that the onset of deconfinement to color superconducting quark matter is likely to occur in neutron stars with masses below 1.0 M⊙.

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“…The idea that DM can be found in neutron star (NS) interiors, exteriors, or in both cases [2,3] has been explored already in [4], where it is meant to be a separated fluid weakly interacting gravitationally with normal matter. Furthermore, examples of microscopic approaches to DM in compact stars that might serve as evidence include axions and their emission resulting in cooling of compacts [5], or sexaquarks [6] which might lead to stellar collapse [7] into a hybrid star with a quark matter (QM) core.…”

Section: Introductionmentioning

confidence: 99%