Gravastars with Kuchowicz metric potential

Ghosh, Shounak; Shee, Dibyendu; Ray, Saibal; Rahaman, Farook; Guha, B. K.

doi:10.1016/j.rinp.2019.102473

Cited by 26 publications

(15 citation statements)

References 65 publications

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“…We have obtained new exact solutions of f (R, T ) field equations by implementing Kuchowicz metric potential to describe the geometries of gravastar. We conclude that the construction of gravastar like stellar model admitting the Kuchowich metric potential in this framework seems to be physically consistent as well as viable similar to GR [34]. Hence, f (R, T ) gravity can provide stable as well as acceptable structures of massive compact objects under the influence of specific metric function same as in GR.…”

Section: Discussionmentioning

confidence: 58%

“…For the intermediate geometry of gravastar, Eqs. (34) and (35) lead to the parameter of EoS at r = R as…”

Section: The Eos Parametermentioning

confidence: 99%

“…For static isotropic matter distribution, it is claimed that the value of redshift parameter should not exceed 2 [49,50]. The expression of surface redshift is presented by [34] Z…”

Section: Surface Redshift Within the Thin-shellmentioning

confidence: 99%

“…This metric function was proposed by Kuchowicz as a non-singular function to discuss the stellar configurations. Ghosh et al [34] employed this metric potential to analyze the features of gravastars in GR. This function provides successful theoretical assistance for massive compact objects corresponding to some particular values of arbitrary constants.…”

Section: Exact Solutions In R + 2αt Modelmentioning

confidence: 99%

“…In the analysis of stellar compact structures, the solutions of the field equations play a significant role. Ghosh et al [34] presented the structure of gravastar by considering the Kuchowicz metric function in GR. They displayed the graphical behavior of various features and found stable structure of gravastar under the influence of their considered singularity free metric function.…”

Section: Introductionmentioning

confidence: 99%

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Impact of Kuchowicz metric function on gravastars in f(R, T) theory

Sharif

Waseem

2020

Eur. Phys. J. Plus

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This paper discusses the configuration of gravitational vacuum star or gravastar with the impact of geometry and matter coupling present in f (R, T) gravity. The gravastar is also conceptualized as a substitute for a black hole which is illustrated by three geometries known as (1) the interior geometry, (2) the intermediate thin-shell and (3) the exterior geometry. For a particular f (R, T) model, we analyze these geometries corresponding to Kuchowicz metric function. We evaluate another metric potential for the interior domain as well as the intermediate shell which is non-singular for both domains. The Schwarzschild metric is adopted to demonstrate the exterior geometry of gravastar, while the numerical values of unknown constants are calculated through boundary conditions. Finally, we discuss different features of gravastar regions like proper length, energy, surface redshift as well as equation of state parameter. We conclude that the gravastar model can be regarded as a successful replacement of the black hole in the context of this gravity.

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Section: Discussionmentioning

confidence: 58%

“…For the intermediate geometry of gravastar, Eqs. (34) and (35) lead to the parameter of EoS at r = R as…”

Section: The Eos Parametermentioning

confidence: 99%

“…For static isotropic matter distribution, it is claimed that the value of redshift parameter should not exceed 2 [49,50]. The expression of surface redshift is presented by [34] Z…”

Section: Surface Redshift Within the Thin-shellmentioning

confidence: 99%

Section: Exact Solutions In R + 2αt Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Impact of Kuchowicz metric function on gravastars in f(R, T) theory

Sharif

Waseem

2020

Eur. Phys. J. Plus

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Dark Energy Star: Physical Constraints on the Bounds

Das

Debnath

Ray

2023

Fortschritte der Physik

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In the present article, we explore a new solution to the Einstein-Maxwell field equations to describe spherically symmetric, charged and anisotropic dark energy stars. The interior of such stars containing two non-interacting fluids like dark and normal matter with a relation that the dark energy density is proportional to the energy density of a isotropic matter. We have used modified chaplygin gas equation to define the dark energy part. Also we have defined the interior space-time through Krori-Barua (KB) space-time and matched it with the exterior Reissner-Nordström space-time. The well-behaveness of the physical attributes have been discussed by plotting graphs for three specific compact objects with respect to our solutions. We conclude that all the physical attributes satisfy the required conditions for viability as well as stability and hence our model can be used to characterize dark energy stars for a set of parametric values belong to the present study.

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Dynamics and Stability via Thin‐Shell of Approximated Black Holes in f(Q)$f(\mathbb {Q})$ Gravity

Javed,

Lin,

Mustafa

et al. 2024

Fortschritte der Physik

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The current study is devoted to exploring the geometrical configuration of a thin‐shell in the background of symmetric teleparallel gravity. For this purpose, the well‐known cut‐and‐paste approach by matching the inner flat and outer newly calculated class of approximated black hole (BH) solutions in symmetric teleparallel gravity are considered, i.e., uncharged, charged, and anti‐de‐Sitter BHs. The dynamical analysis of thin‐shell configuration by adopting the massive and massless scalar field via Klein‐Gordon's equation of motion is discussed. The effective potential and proper time derivative of shell radius for both massive and massless scalar shells are used to discuss the collapse, expansion, and oscillatory behavior. The stable configuration of thin‐shell is observed through the linearized radial perturbation approach with a phantomlike equation of state, i.e., quintessence, dark energy, and phantom energy. It is noted that stable/unstable behavior of thin‐shell is found after the expected position of the event horizon of an exterior manifold. It is concluded that the stability of a thin‐shell is greater for BH with cosmological constant as compared to the uncharged and charged BHs.

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Gravastars with Kuchowicz metric potential

Cited by 26 publications

References 65 publications

Impact of Kuchowicz metric function on gravastars in f(R, T) theory

Impact of Kuchowicz metric function on gravastars in f(R, T) theory

Dark Energy Star: Physical Constraints on the Bounds

Dynamics and Stability via Thin‐Shell of Approximated Black Holes in f(Q)$f(\mathbb {Q})$ Gravity

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