Strange stars in the presence of quintessence

Estevez-Delgado, Joaquin; Campuzano, Elivet Aguilar; Ceballos, Joel Arturo Rodriguez; Murguía, Aurelio Tamez; Cabrera, Jose Vega

doi:10.1140/epjp/s13360-020-00212-2

Cited by 20 publications

(10 citation statements)

References 28 publications

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“…So, this shows that the internal structure of the stars is influenced by the compactness of the star, since as we know the state equations are a consequence of the type of matter and the interaction between them, and in our case, of the specific value of µ, this is a considerable difference of our work with respect to other. 32,35 As well as that, in our model, objects with a greater compactness are characterized because µ should be close to 1, due to this, the speed of sound would be very close to the speed of light. This generates some questions on the effect of the quintessence when it interacts with the matter.…”

Section: Discussionmentioning

confidence: 58%

“…38,39 In our case, the parameter µ ∈ (0, 1] has an interval of values, which is consistent with the possibility that the matter is formed by a mixture of particles like quarks, neutrons and electrons and not only by one type of them. On the other hand, as it has been argued in a previous investigation report 35 and following this idea, other investigation works have been written, 32,34 the structure of the state equation for the tangential pressure is proposed to describe how the quintessence could disturb a perfect fluid.…”

Section: The Field Equations and Physical Conditionsmentioning

confidence: 97%

“…It is this characteristic which allows that a geometry associated to a perfect fluid in absence of quintessence is applicable to the anisotropic case with quintessence. 32,34,35 Systems (4) Quintessences compact star with Durgapal potential equivalent form as follows 35 :…”

Section: The Field Equations and Physical Conditionsmentioning

confidence: 99%

“…Furthermore, in previous works, it has already been shown that the compactness rate of the initial model with perfect fluid and its respective case for the anisotropic fluid with quintessence has the same function of the compactness rate and its maximum value is of the same order. 32,34,35 The form of the metric coefficients of the Durgapal metric for n = 5, is y(r) = (1 + ar 2 )…”

Section: The Solution and Its Analysismentioning

confidence: 99%

“…25,26 Some works about compact stars have already approached the possibility of quintessence and ordinary matter, the quintessence is described mainly by a fluid with radial and tangential pressures linked to the quintessence described by P rq = −c 2 ρ q and P tq = (1 + 3w)c 2 ρ q /2 with −1 < w < −1/3 where ρ q represents the density of the quintessence matter, these equations were proposed initially for the case of black holes with quintessence, 27 meanwhile for the ordinary matter, there have been different proposed sources. 28,29 Within the variety of compact stars with quintessence, [30][31][32] one of the most approached is that associated to the MIT Bag model, 33,34 for this case, starting from a state equation associated to the ordinary matter and considering the effect of the quintessence, it has been shown that the geometry of the solutions for Einstein's equations with perfect fluid works for describing compact stars with quintessence. 35 However, it is to be expected that the ordinary matter that conforms a star is not only constituted by quarks and that depending on its mass, radius, density or compactness its state equation may differ.…”

Section: Introductionmentioning

confidence: 99%

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Quintessences compact star with Durgapal potential

Estevez-Delgado

Murguía

et al. 2020

Mod. Phys. Lett. A

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A compact star model formed by quintessence and ordinary matter is presented, both sources have anisotropic pressures and are described by linear state equations, also the state equation of the tangential pressure for the ordinary matter incorporates the effect of This is an Open Access article published by World Scientific Publishing Company. It is distributed under the terms of the Creative Commons Attribution 4.0 (CC BY) License which permits use, distribution and reproduction in any medium, provided the original work is properly cited.* Corresponding author. 2050144-1 Mod. Phys. Lett. A 2020.35. Downloaded from www.worldscientific.com by 44.224.250.200 on 07/11/20. Re-use and distribution is strictly not permitted, except for Open Access articles. G. Estevez-Delgado et al.the quintessence. It is shown that depending on the compactness of the star u = GM/c 2 R the constant of proportionality µ between the density of the ordinary matter and the radial pressure, Pr = µc 2 (ρ − ρ b ), has an interval of values which is consistent with the possibility that the matter is formed by a mixture of particles like quarks, neutrons and electrons and not only by one type of them. The geometry is described by the Durgapal metric for n = 5 and each one of the pressures and densities is positive, finite and monotonic decreasing, as well as satisfying the condition of causality and of stability v 2 t − v 2 r < 0, which makes our model physically acceptable. The maximum compactness that we have is u ≤ 0.28551, so we can apply our solution considering the observational data of mass and radii M = (2.01 ± 0.04) M ⊙ , R ∈ [12.062, 12.957] km which generate a compactness 0.22448 ≤ u ≤ 0.25448 associated to the star PSR J0348 + 0432. In this case, the interval of µ ∈ [0.78055, 1] and its maximum central density ρc and in the surface ρ b of the star are ρc = 7.0387 × 10 17 kg/m 3 and ρ b = 4.6807 × 10 17 kg/m 3 , respectively, meanwhile the central density of the quintessence ρqc = 3.4792 × 10 16 kg/m 3 .

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Section: Discussionmentioning

confidence: 58%

Section: The Field Equations and Physical Conditionsmentioning

confidence: 97%

Section: The Field Equations and Physical Conditionsmentioning

confidence: 99%

Section: The Solution and Its Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Quintessences compact star with Durgapal potential

Estevez-Delgado

Murguía

et al. 2020

Mod. Phys. Lett. A

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Ricci inverse anisotropic stellar structures

Shamir

Ahmad

Mustafa

et al. 2023

Chinese Journal of Physics

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Determination of the charge for strange stars

Estevez-Delgado

2022

Class. Quantum Grav.

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Starting from the proposal of a physically acceptable model to represent the interior of compact stars, in which their interior is formed by strange matter distribution described by a charged ﬂuid with anisotropic pressure with a MIT Bag equation of state for the radial pressure Pr = (c2 ρ − 4Bg)/3 and metric functions given by the Estevez - Delgado geometry that describes a regular, static and spherically symmetric space-time, we determine the possible charge of some strange stars or candidates for which we know in an observational manner their radius and mass. As they are EXO 1785- 248, SAX J1808.4 -3658, SMC X -4, LMC X -4, Her X -1 and 4U 1538-52. The values of the Bag constant, Bg, are found between 119.8Mev/fm3 and 176.41Mev/fm3. Meanwhile the interval of the electric charge is found between 1.5453 × 1018C and 7.6271 × 10 19 C, the minimum corresponds to the star Her X-1 and the maximum to the star SMCX - 4. Also, we show that for each ﬁxed value of compactness u = GM/c2 R, we have that for greater values of the Bag constant the net charge diminishes and as the compactness increases the associated Bag constant increases as well.

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Strange stars in the presence of quintessence

Cited by 20 publications

References 28 publications

Quintessences compact star with Durgapal potential

Quintessences compact star with Durgapal potential

Ricci inverse anisotropic stellar structures

Determination of the charge for strange stars

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