Chaplygin strange stars in presence of quintessence

Estevez-Delgado, Joaquin; Duran, Modesto Pineda; Cleary-Balderas, Arthur; Maya, Noel Enrique Rodríguez; Peña, José Martínez

doi:10.1142/s0217732321502138

Cited by 12 publications

(8 citation statements)

References 35 publications

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“…On the other hand, at astrophysics level, compact stars obeying the EoS (28) have been investigated by several authors, see for example Refs. [38,41,[43][44][45]. In this work we will adopt values of A and B for which appreciable changes in the mass-radius diagram can be visualized in order to compare our theoretical results with observational measurements of massive pulsars.…”

Section: Equation Of State and Anisotropy Modelmentioning

confidence: 99%

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Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Pretel

2023

Eur. Phys. J. C

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We construct dark energy stars with Chaplygin-type equation of state (EoS) in the presence of anisotropic pressure within the framework of Einstein gravity. From the classification established by Iyer et al. (Class Quantum Grav 2:219, 1985), we discuss the possible existence of isotropic dark energy stars as compact objects. However, there is the possibility of constructing ultra-compact stars for sufficiently large anisotropies. We investigate the stellar stability against radial oscillations, and we also determine the moment of inertia and tidal deformability of these stars. We find that the usual static criterion for radial stability $$dM/d\rho _c >0$$ d M / d ρ c > 0 still holds for dark energy stars since the squared frequency of the fundamental pulsation mode vanishes at the critical central density corresponding to the maximum-mass configuration. The dependence of the tidal Love number on the anisotropy parameter $$\alpha $$ α is also examined. We show that the surface gravitational redshift, moment of inertia and dimensionless tidal deformability undergo significant changes due to anisotropic pressure, primarily in the high-mass region. Furthermore, in light of the detection of gravitational waves GW190814, we explore the possibility of describing the secondary component of such event as a stable dark energy star in the presence of anisotropy.

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Section: Equation Of State and Anisotropy Modelmentioning

confidence: 99%

“…For further stellar models with dark energy we also refer the reader to Refs. [40][41][42][43][44][45][46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Pretel

2023

Eur. Phys. J. C

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“…guarantees the absence of event horizons. In addition of this the functions (9) that describe the geometry were initially proposed to model anisotropic chargeless and charged perfect fluid objects [74], afterwards they were employed for the case of a charged anisotropic fluid with a state equation type Chaplygin [76] and with quintessence sources of matter [77], as well as for a linear equation of state [78] and non linear equation of state [79].…”

Section: Basic Equationsmentioning

confidence: 99%

“…It is also applicable in alternative gravitational theory models [80,81]. This same geometry allows for the description of models that are differentiated for the type of sources of matter in situations with or without equation of state [74,[76][77][78][79][80][81]. The different models proposed were applied to describe the interior of many stellar objects for which their observational data is known and also it has been shown that the geometry is regular and absent of event horizon, motivated by this, in this report the focus will be centered in the construction of a model, the description of it's behaviour and it's application to determining the possible values of the charge considering some values of the Bag constant inside of the admissible interval of it.…”

Section: Basic Equationsmentioning

confidence: 99%

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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“…For further stellar models with dark energy we also refer the reader to Refs. [40][41][42][43][44][45][46][47][48].…”

Section: Introductionmentioning

confidence: 99%

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Pretel¹

2023

Preprint

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We construct dark energy stars with Chaplygin-type equation of state (EoS) in the presence of anisotropic pressure within the framework of Einstein gravity. From the classification established by Iyer et al. [Class. Quantum Grav. 2, 219 (1985)], we discuss the possible existence of isotropic dark energy stars as compact objects. However, there is the possibility of constructing ultra-compact stars for sufficiently large anisotropies. We investigate the stellar stability against radial oscillations, and we also determine the moment of inertia and tidal deformability of these stars. We find that the usual static criterion for radial stability dM/dρc > 0 still holds for dark energy stars since the squared frequency of the fundamental pulsation mode vanishes at the critical central density corresponding to the maximum-mass configuration. The dependence of the tidal Love number on the anisotropy parameter α is also examined. We show that the surface gravitational redshift, moment of inertia and dimensionless tidal deformability undergo significant changes due to anisotropic pressure, primarily in the high-mass region. Furthermore, in light of the detection of gravitational waves GW190814, we explore the possibility of describing the secondary component of such event as a stable dark energy star in the presence of anisotropy.

show abstract

Chaplygin strange stars in presence of quintessence

Cited by 12 publications

References 35 publications

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Determination of the charge for strange stars

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

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