Relativistic strange stars in Tolman–Kuchowicz spacetime

Biswas, S. N.; Shee, Dibyendu; Ray, Saibal; Rahaman, Farook; Guha, B. K.

doi:10.1016/j.aop.2019.05.004

Cited by 48 publications

(17 citation statements)

References 115 publications

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“…eir evolution in both f(R) models for CS1 candidate represents positive nature within the entire region of the star and gradually increases with the increase of the radial parameter r (Figure 20 Figure 20: Combined graphical behaviors with magnified images of the metric potentials (e ξ(r) and e ζ(r) ) versus r for compact object (CS1) SAX J 1808.4-3658 with their respective unknown arbitrary constant values given in Tables 1 and 2 profile of energy density, radial pressure, tangential pressure, and electric field suggests positive evolution throughout the whole interior distribution of the fluid sphere and remains regular (finite) at every interior point of the star. One important point that should be necessarily discussed is that the numerical values of central density are greater than the surface density (Tables 1-6), which actually expected the very massive strange quark star objects [107][108][109][110]. We have also noted that the radial pressure sharply dies out at the boundary surface of the sphere, but tangential pressure does not exactly vanish, which clearly signifies the spheroidal nature for our CS1 candidate [112][113][114].…”

Section: Advances In Astronomymentioning

confidence: 89%

“…It is seen from Figure 1 that each plot of the energy density shows nonnegative nature within the entire region of the star, and it suggests maximum behavior at the center and minimum towards the boundary surface of the sphere. Apart from this description, one important point to discuss is that the numerical value of the central density is up most in competition of the surface density of the compact star candidates (Tables 1-6), which is actually the property of massive strange quark stellar objects [107][108][109][110]. Figures 2 and 3 show the evolutionary nature of the radial and transverse pressures through graphical analysis by using two well-known f(R) models.…”

Section: Evolution Of Matter Density Pressure and Electric Fieldmentioning

confidence: 99%

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Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Nazar

Abbas

2021

Advances in Astronomy

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In the present article, we have investigated a new family of nonsingular solutions of static relativistic compact sphere which incorporates the characteristics of anisotropic fluid and electromagnetic field in the context of minimally coupled f R theory of gravity. The strange matter MIT bag model equation of state (EoS) has been considered along with the usual forms of the Karori–Barua KB metric potentials. For this purpose, we derived the Einstein–Maxwell field equations in the assistance of strange matter EoS and KB type ansatz by employing the two viable and cosmologically well-consistent models of f R = R + γ R 2 and f R = R + γ R R + α R 2 . Thereafter, we have checked the physical acceptability of the proposed results such as pressure, energy density, energy conditions, TOV equation, stability conditions, mass function, compactness, and surface redshift by using graphical representation. Moreover, we have investigated that the energy density and radial pressure are nonsingular at the core or free from central singularity and always regular at every interior point of the compact sphere. The numerical values of such parameters along with the surface density, charge to radius ratio, and bag constant are computed for three well-known compact stars such as CS1 SAXJ 1808 . 4 − 3658 ( x ˜ = 7.07 km , CS2 VelaX − 1 x ˜ = 9.56 km , and CS3 4U1820 − 30 x ˜ = 10 km and are presented in Tables 1–6. Conclusively, we have noticed that our presented charged compact stellar object in the background of two well-known f R models obeys all the necessary conditions for the stable equilibrium position and which is also perfectly fit to compose the strange quark star object.

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Section: Advances In Astronomymentioning

confidence: 89%

Section: Evolution Of Matter Density Pressure and Electric Fieldmentioning

confidence: 99%

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Nazar

Abbas

2021

Advances in Astronomy

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“…Several researchers from the field of general relativity as well as in the field of modified gravity have used the above metric potentials earlier. In connection with the MIT Bag model equation of state, Biswas et al [45] used this metric potentials to obtain a strange star structure. Under Einstein's general theory of relativity, in the presence of the cosmological constant Λ (where Λ=Λ(r)), Jasim et al [46] examined a unique model for spherically symmetry of anisotropic strange stars.…”

Section: Interior Spacetime and Field Equationsmentioning

confidence: 99%

Dark Energy Stars in Tolman-Kuchowicz spacetime in the context of Einstein Gravity

Bhar

2022

Preprint

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Dark energy is the component in the present Universe with the greatest abundance, and it is responsible for the accelerating expansion of the Universe. As a result, dark energy is likely to interact with any compact astrophysical object [Muhammad F.A.R. Sakti and Anto Sulaksono, Phys. Rev. D 103, 084042 (2021)]. In present paper, we propose a model for a dark energy star made up of dark and ordinary matter in which the density of dark energy is proportional to the density of isotropic perfect fluid matter. In the context of general relativity, the model is derived in the curved Tolman-Kuchowicz spacetime geometry [Tolman, Phys Rev 55:364, (1939); Kuchowicz, Acta Phys Pol 33:541, (1968)]. Here, we look at how dark energy affects stellar mass, compactness, and equilibrium etc. The physical parameters of the model e.g., pressure, density, mass function, surface redshift etc. are investigated, and the stability of stellar configuration is studied in detail. The model has interesting properties because it meets all energy criteria and is free from central singularities. The maximum allowable mass has been obtained from our model with the help of M − R diagram. We analyse many physical properties of the model and checked that it meets all regularity constraints, is stable, and therefore physically realistic.

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“…The simple linear EoS which expresses the pressure as a linear function of the fluid density ( p r = αρ) where α ≥ is a constant has been extended to include α < 0 used in modeling so-called dark stars and phantom fields. The MIT Bag model EoS has gained popularity amongst researchers and has been successfully utilised to model compact objects in classical GR and modified gravity theories [36,37]. The quadratic EoS, polytropic EoS and Chaplygin gas EoS have also led to physically reasonable models of static stars [38][39][40].…”

Section: Introductionmentioning

confidence: 99%

Anisotropic stars via embedding approach in Brans–Dicke gravity

et al. 2021

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In the present article, the solution of the Einstein–Maxwell field equations in the presence of a massive scalar field under the Brans-Dicke (BD) gravity is obtained via embedding approach, which describes a charged anisotropic strange star model. The interior spacetime is described by a spherically symmetric static metric of embedding class I. This reduces the problem to a single-generating function of the metric potential which is chosen by appealing to physics based on regularity at each interior point of the stellar interior. The resulting model is subjected to rigorous physical checks based on stability, causality and regularity for particular object PSR J1903+327. We also show that our solutions describe compact objects such as PSR J1903+327; Cen X-3; EXO 1785-248 and LMC X-4 to an excellent approximation. Novel results of our investigation reveal that the scalar field leads to higher surface charge densities which in turn affects the compactness and upper and lower values imposed by the modified Buchdahl limit for charged stars. Our results also show that the electric field and scalar field which originate from entirely different sources couple to alter physical characteristics such as mass-radius relation and surface redshift of compact objects. This superposition of the electric and scalar fields is enhanced by an increase in the BD coupling constant, $$\omega _{BD}$$ ω BD .

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Relativistic strange stars in Tolman–Kuchowicz spacetime

Cited by 48 publications

References 115 publications

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Dark Energy Stars in Tolman-Kuchowicz spacetime in the context of Einstein Gravity

Anisotropic stars via embedding approach in Brans–Dicke gravity

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Relativistic strange stars in Tolman–Kuchowicz spacetime

Cited by 48 publications

References 115 publications

Model of Charged Anisotropic Strange Stars in Minimally Coupled f R Gravity

Model of Charged Anisotropic Strange Stars in Minimally Coupled f R Gravity

Dark Energy Stars in Tolman-Kuchowicz spacetime in the context of Einstein Gravity

Anisotropic stars via embedding approach in Brans–Dicke gravity

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Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity

Model of Charged Anisotropic Strange Stars in Minimally Coupled $f (R)$ Gravity