Dark matter and dark energy from quark bag model

Brilenkov, Maxim; Eingorn, Maxim; Jenkovszky, L. L.; Zhuk, Alexander

doi:10.1088/1475-7516/2013/08/002

Cited by 40 publications

(45 citation statements)

References 35 publications

(61 reference statements)

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“…It is observed that to describe a stellar model made of strange quark matter well known MIT bag EOS can be considered under such a situation. Successful use of the MIT bag EOS to describe strange quark stars the following recent works are available in the literature [31,32,33,34,35,36,37,38]. This type of simplest form of EOS is very useful to study equilibrium configuration of a compact stellar object made of only up, down and strange quarks even in the framework of general relativity without invoking any quantum mechanical particle physics aspect.…”

Section: Introductionmentioning

confidence: 99%

Relativistic model for anisotropic strange stars

et al. 2017

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In this article, we attempt to find a singularity free solution of Einstein's field equations for compact stellar objects, precisely strange (quark) stars, considering Schwarzschild metric as the exterior spacetime. To this end, we consider that the stellar object is spherically symmetric, static and anisotropic in nature and follows the density profile given by Mak and Harko (2002), which satisfies all the physical conditions. To investigate different properties of the ultra-dense strange stars we have employed the MIT bag model for the quark matter. Our investigation displays an interesting feature that the anisotropy of compact stars increases with the radial coordinate and attains Preprint submitted to Annals of Physics October 19, 2017 its maximum value at the surface which seems an inherent property for the singularity free anisotropic compact stellar objects. In this connection we also perform several tests for physical features of the proposed model and show that these are reasonably acceptable within certain range. Further, we find that the model is consistent with the energy conditions and the compact stellar structure is stable with the validity of the TOV equation and Herrera cracking concept. For the masses bellow the maximum mass point in mass vs radius curve the typical behavior achieved within the framework of general relativity. We have calculated the maximum mass and radius of the strange stars for the three finite values of bag constant B g .

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Section: Introductionmentioning

confidence: 99%

Relativistic model for anisotropic strange stars

et al. 2017

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“…On the other hand, the proposal by [1], which can be considered as part of the stream of unified dark matter models, has been suggested to explain the nature of DM and the present cosmic acceleration. Such suggestion arises from the hypothesis that a small part of quarks and gluons did not yield to hadronization, and resisted either as isolated aggregates of quark-gluon nuggets (QNs) or as a perfect fluid in the form of a quark-gluon plasma (QGP) (uniformly spread on cosmological scales).…”

Section: Introductionmentioning

confidence: 99%

“…A recent work [42] explored the possibility that the QGP fluid acted as DM in galactic halos concluding that the corresponding rotation curves were reasonable. At the cosmological level, a QGP fluid was first considered to mimic DM in [1].…”

Section: Introductionmentioning

confidence: 99%

Observational constraints on the unified dark matter and dark energy model based on the quark bag model

Montiel¹,

Salzano²,

Lazkoz³

2014

Physics Letters B

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In this work we investigate if a small fraction of quarks and gluons, which escaped hadronization and survived as a uniformly spread perfect fluid, can play the role of both dark matter and dark energy. This fluid, as developed in [1], is characterized by two main parameters: β, related to the amount of quarks and gluons which act as dark matter; and γ, acting as the cosmological constant. We explore the feasibility of this model at cosmological scales using data from type Ia Supernovae (SNeIa), Long Gamma-Ray Bursts (LGRB) and direct observational Hubble data. We find that: (i) in general, β cannot be constrained by SNeIa data nor by LGRB or H(z) data; (ii) γ can be constrained quite well by all three data sets, contributing with ≈ 78% to the energy-matter content; (iii) when a strong prior on (only) baryonic matter is assumed, the two parameters of the model are constrained successfully.

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“…There is a number of interesting modifications [1,2,[26][27][28][29][30]. In our paper [8], we considered two possible forms of the equation of state. The corresponding total background pressure 2 and energy density of all nuggets in the Universe, as well as their temperature, read, respectively,…”

Section: Quark-gluon Nuggetsmentioning

confidence: 99%

Scalar perturbations in cosmological models with quark nuggets

et al. 2014

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In this paper we consider the Universe at the late stage of its evolution and deep inside the cell of uniformity. At these scales, the Universe is filled with inhomogeneously distributed discrete structures (galaxies, groups and clusters of galaxies). Supposing that a small fraction of colored objects escaped hadronization and survived up to now in the form of quark-gluon nuggets (QNs), and also taking into account radiation, we investigate scalar perturbations of the FRW metrics due to inhomogeneities of dustlike matter as well as fluctuations of QNs and radiation. In particular, we demonstrate that the nonrelativistic gravitational potential is defined by the distribution of inhomogeneities/fluctuations of both dustlike matter and QNs. Consequently, QNs can be distributed around the baryonic inhomogeneities (e.g., galaxies) in such a way that it can solve the problem of the flatness of the rotation curves. We also show that the fluctuations of radiation are caused by both the inhomogeneities in the form of galaxies and the fluctuations of quark-gluon nuggets. Therefore, if QNs exist, the CMB anisotropy should contain also the contributions from QNs. Additionally, the spatial distribution of the radiation fluctuations is defined by the gravitational potential. All these results look physically reasonable.

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Dark matter and dark energy from quark bag model

Cited by 40 publications

References 35 publications

Relativistic model for anisotropic strange stars

Relativistic model for anisotropic strange stars

Observational constraints on the unified dark matter and dark energy model based on the quark bag model

Scalar perturbations in cosmological models with quark nuggets

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