The measure of complexity in charged celestial bodies in <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline" id="d1e22" altimg="si7.svg"><mml:mrow><mml:mi>f</mml:mi><mml:mrow><mml:mo>(</mml:mo><mml:mi>R</mml:mi><mml:mo>,</mml:mo><mml:mi>T</mml:mi><mml:mo>,</mml:mo><mml:msub><mml:mrow><mml:mi>R</mml:mi></mml:mrow><mml:mrow><mml:mi>μ</mml:mi><mml:mi>ν</mml:mi></mml:mrow></mml:msub><mml:msup><mml:mrow><mml:mi>T</mml:mi></mml:mrow><mml:mrow><mml:mi>μ</mml:mi><mml:mi>ν</mml:mi></mml:mrow><

Yousaf, Z.; Bhatti, M. Z.; Naseer, Tayyab; Ahmad, Iftikhar

doi:10.1016/j.dark.2020.100581

Cited by 46 publications

(23 citation statements)

References 64 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Using (19) we can define the velocity U of the collapsing fluid as the variation of the proper radius with respect to proper time, i.e.…”

Section: B Kinematical Variables and The Mass Functionmentioning

confidence: 99%

“…The presented arguments in [2] strongly suggested that the homologous condition seemed to be the most suitable to describe the simplest mode of evolution. The applications of this concept including systems with different kind of symmetry and/or other theories of gravity, may be found in [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21] and references therein.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Quasi-homologous evolution of self-gravitating systems with vanishing complexity factor

2020

View full text Add to dashboard Cite

We investigate the evolution of self-gravitating either dissipative or non-dissipative systems satisfying the condition of minimal complexity, and whose areal radius velocity is proportional to the areal radius (quasi-homologous condition). Several exact analytical models are found under the above mentioned conditions. Some of the presented models describe the evolution of spherically symmetric dissipative fluid distributions whose center is surrounded by a cavity. Some of them satisfy the Darmois conditions whereas others present shells and must satisfy the Israel condition on either one or both boundary surfaces. Prospective applications of some of these models to astrophysical scenarios are discussed.

show abstract

“…Using (19) we can define the velocity U of the collapsing fluid as the variation of the proper radius with respect to proper time, i.e.…”

Section: B Kinematical Variables and The Mass Functionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Quasi-homologous evolution of self-gravitating systems with vanishing complexity factor

2020

View full text Add to dashboard Cite

show abstract

“…Sharif and Waseem [21,22] studied certain physical attributes of massive isotropic/anisotropic configured stars and checked their stable regions. Yousaf et al [23][24][25][26][27] computed several structure scalars for static and non-static cases which are related with the fundamental properties of matter distribution. These scalars help to illustrate the composition and expansion of self-gravitating stellar configuration.…”

Section: Introductionmentioning

confidence: 99%

Study of Decoupled Anisotropic Solutions in f(R, T, RρηTρη) Theory

Naseer

Sharif

2022

Universe

View full text Add to dashboard Cite

In this paper, we consider isotropic solution and extend it to two different exact well-behaved spherical anisotropic solutions through minimal geometric deformation method in f(R,T,RρηTρη) gravity. We only deform the radial metric component that separates the field equations into two sets corresponding to their original sources. The first set corresponds to perfect matter distribution while the other set exhibits the effects of additional source, i.e., anisotropy. The isotropic system is resolved by assuming the metric potentials proposed by Krori-Barua while the second set needs one constraint to be solved. The physical acceptability and consistency of the obtained solutions are analyzed through graphical analysis of effective matter components and energy bounds. We also examine mass, surface redshift and compactness of the resulting solutions. For particular values of the decoupling parameter, our both solutions turn out to be viable and stable. We conclude that this curvature-matter coupling gravity provides more stable solutions corresponding to a self-gravitating geometry.

show abstract

“…Then, Herrera et al [52] generalized their concept for dynamical self-gravitating systems. Recently, Sharif and Majid [53] and Yousaf et al [54,55] modified their results in the Brans-Dicke theory and f (R, T, R µν T µν ) gravity, respectively and analyzed the role of modified terms in the formulation of CF.…”

Section: Introductionmentioning

confidence: 99%

Definition of Complexity Factor for Self-Gravitating Systems in Palatini $f(R)$ Gravity

Yousaf

2020

Preprint

Self Cite

View full text Add to dashboard Cite

The aim of this paper is to explore the complexity factor for those self-gravitating relativistic spheres whose evolution proceeds non-dynamically. We are adopting the definition of CF mentioned in [50], modifying it to the static spherically symmetric case, within the framework of a modified gravity theory (the Palatini f (R) theory). In this respect, we have considered radial dependent anisotropic matter content coupled with spherical geometry and determined the complexity factor involved in the patterns of radial evolution. We shall explore the field and a well-known Tolman-Oppenheimer-Volkoff equations. After introducing structure scalars from the orthogonal decomposition of the Riemann tensor, we shall calculate complexity factor. An exact analytical model is presented by considering firstly ansatz provided by Gokhroo and Mehra. The role of matter variables and f (R) terms are analyzed in the structure formation as well as their evolution through a complexity factor.

show abstract

The measure of complexity in charged celestial bodies in f(R,T,RμνTμν<

Cited by 46 publications

References 64 publications

Quasi-homologous evolution of self-gravitating systems with vanishing complexity factor

Quasi-homologous evolution of self-gravitating systems with vanishing complexity factor

Study of Decoupled Anisotropic Solutions in f(R, T, RρηTρη) Theory

Definition of Complexity Factor for Self-Gravitating Systems in Palatini $f(R)$ Gravity

Contact Info

Product

Resources

About