A regular perfect fluid model for dense stars

Estevez-Delgado, Gabino; Estevez-Delgado, Joaquin; Paulin-Fuentes, Jorge Mauricio; García, Nadiezhda Montelongo; Duran, Modesto Pineda

doi:10.1142/s0217732319501153

Cited by 30 publications

(11 citation statements)

References 36 publications

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“…which matches the restriction that we have between (B, y) for the case of a model formed with only a perfect fluid [49].…”

Section: The Field Equationssupporting

confidence: 83%

“…Theorem 1 could be applied to the set of known regular solutions for a perfect fluid [49,[52][53][54][55] and we obtain for each one of these a model that tentatively describes stars formed by quintessence and MIT Bag matter. The existence of these with the equations for the radial and tangential pressures given by (7) and (8) is a new theoretical proposal presented in this work., Its possible physical existence is justified by the astrophysics observations related to the accelerated expansion of the universe.…”

Section: The Field Equationsmentioning

confidence: 99%

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On quintessence star model and strange star

Estevez-Delgado

2020

Eur. Phys. J. C

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The astronomical observations on the accelerated expansion of the universe generate the possibility that the internal matter of the stars is not only formed by ordinary matter but also by matter with negative pressure. We discuss the existence of stars formed by the coexistence of two types of fluids, one associated to quintessence dark matter described by the radial and tangential pressures $$(P_{rq},P_{tq})$$ ( P rq , P tq ) and the density $$\rho _{q}$$ ρ q characterized by a parameter $$-1<w<-\frac{1}{3}$$ - 1 < w < - 1 3 and ordinary matter described by an anisotropic fluid with radial pressure of a strange star given by the MIT Bag model $$P_r=\frac{1}{3}(c^2\rho -4B_g)$$ P r = 1 3 ( c 2 ρ - 4 B g ) and tangential pressure $$P_t=\frac{1}{3}(c^2\rho -4B_g)-\frac{3}{2}(1+w)c^2\rho _q$$ P t = 1 3 ( c 2 ρ - 4 B g ) - 3 2 ( 1 + w ) c 2 ρ q , in which the effect is reflected of the quintessence dark matter over the ordinary matter. Via a theorem we show that the geometry that describes this interaction is equivalent to that of a perfect fluid with ordinary matter. Taking as geometry the one associated with a model for neutron stars, a physically acceptable and stable model is obtained. The application to the star Her X-1, as a candidate to a strange quark star, generates for us a value of the MIT Bag constant $$B_g = 97.0048\,\mathrm{Mev}/\mathrm{fm}^3$$ B g = 97.0048 Mev / fm 3 , which is found to be inside the expected interval.

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“…which matches the restriction that we have between (B, y) for the case of a model formed with only a perfect fluid [49].…”

Section: The Field Equationssupporting

confidence: 83%

Section: The Field Equationsmentioning

confidence: 99%

On quintessence star model and strange star

Estevez-Delgado

2020

Eur. Phys. J. C

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“…In some works presented in the last century, there were some solutions found for the equation systems (3)-(5), considering the form of the gravitational potential 9 g tt = (1 + ar 2 ) n and recently it has been shown that different choices allow for the description of compact objects. [10][11][12] In this work, we assume the form of that gravitational potential as…”

Section: Perfect Fluid Solutionmentioning

confidence: 99%

“…Our focus does not assume a state equation, but instead, the way to describe the interior of the star starting from the proposal of a form of the metric potential y(r) and of the solution of the isotropy equation in the pressures. As such, the adiabatic index is determined from the form obtained of the density and the pressure given by (11) and (12), respectively. Although the expression for γ is not presented here, due to its length, its behavior is shown in Fig.…”

Section: An Interior Solution With Perfect Fluidmentioning

confidence: 99%

“…Some solutions that are physically acceptable have been employed to describe stars. 8,[10][11][12][13][14] Recently, with the development of other gravitation theories, the themes that could only be approached with the general theory of relativity have been extended to other theories, the analysis of internal solutions has not been the exception. In the F (R) theory, the existence of neutron stars and quark stars has been studied, 15,16 as well as the stability.…”

Section: Introductionmentioning

confidence: 99%

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An interior solution with perfect fluid

et al. 2020

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Starting from the construction of a solution for Einstein’s equations with a perfect fluid for a static spherically symmetric spacetime, we present a model for stars with a compactness rate of [Formula: see text]. The model is physically acceptable, that is to say, its geometry is non-singular and does not have an event horizon, pressure and speed of sound are bounded functions, positive and monotonically decreasing as function of the radial coordinate, also the speed of sound is lower than the speed of light. While it is shown that the adiabatic index [Formula: see text], which guarantees the stability of the solution. In a complementary manner, numerical data are presented considering the star PSR J0737-3039A with observational mass of [Formula: see text], for the value of compactness [Formula: see text], which implies the radius [Formula: see text] and the range of the density [Formula: see text] [Formula: see text], where [Formula: see text] and [Formula: see text] are the central density and the surface density, respectively. This range is consistent with the expected values; as such, the model presented allows to describe this type of stars.

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Fluids in Equilibrium and Hydrodynamics

Battaglia

Termini

Fazio

2023

The International Handbook of Physics Education Research: Learning Physics

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Foundations and applications of fluid mechanics are relevant in several scientific and technical fields, like physics, engineering, medicine, environmental sciences, and mathematics. The study of fluid mechanics is included in several school curricula worldwide, and as early as the 1980s, there has been growing interest in the Physics Education Research (PER) field about the subject. Several PER researchers have tried to understand how students' conceptions of liquids or gases can affect the effectiveness of instruction, and many literature pieces are available that discuss different possible ways of teaching the concepts related to the equilibrium of fluids and hydrodynamics. They mainly aim to shed light on how to facilitate student learning of fluid mechanics foundations and applications and foster student broad awareness of how this subject plays a role in so many different disciplines. In this chapter, we discuss some relevant examples of these publications to understand how educational research has contributed to the knowledge of teaching/learning of fluid mechanics, how it has evolved in terms of analysis of student learning in this subject, and methodologies and tools proposed and trialed.

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A regular perfect fluid model for dense stars

Cited by 30 publications

References 36 publications

On quintessence star model and strange star

On quintessence star model and strange star

An interior solution with perfect fluid

Fluids in Equilibrium and Hydrodynamics

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