Anisotropic stars in $$f({\textit{G}},{\textit{T}})$$ f ( G ,
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Anisotropic stars in f (G, T) gravity under class I space-time S. K. Maurya1,a , Ksh. Newton Singh2,b , Abdelghani Errehymy3,c , Mohammed Daoud4,5,d 1 Department of Mathematical and Physical Sciences, College of Arts and Science, University of Nizwa,
Nizwa, Sultanate of Oman
2 Department of Physics, National Defence Academy, Khadakwasla, Pune 411023, India 3 Laboratory of High Energy Physics and Condensed Matter (LPHEMaC), Department of Physics, Faculty of
Sciences Aïn Chock, Hassan II University of Casablanca, B.P. 5366 Maarif, 20100 Casablanca, Morocco
4 Department of Physics, Faculty of Sciences, University of Ibn Tofail, B.P. 133, 14000 Kenitra, Morocco 5 Abdus Salam International Centre for Theoretical Physics, 34151 Miramare, Trieste, Italy
Received: 22 August 2020 / Accepted: 5 October 2020 © Società Italiana di Fisica and Springer-Verlag GmbH Germany, part of Springer Nature 2020
Abstract In this paper, we studied the possible existence of anisotropic spherically symmetric solutions in the arena of modified f (G, T)-gravity theory. To supply exact solutions of the field equations, we consider that the gravitational Lagrangian can be expressed as the generic function of the quadratic Gauss–Bonnet invariant G and the trace of the stress–energy tensor T, i.e., f (G, T) = G2 + χT, where χ is a coupling parameter. We ansatz the gravitational ) potential: grr ≡ eλ(r ) from the relationship quasi-local mass function, e−λ = 1 − 2m(r r , and ν(r ) via the embedding class one procedure. we obtained the gravitational potential: gtt ≡ e In this regard, we investigated that the new solution is well analyzed and well comported through various physical and mathematical tests, which confirmed the physical viability and the stability of the system. The present investigation uncovers that the f (G, T)-gravity via embedding class one approach is a well acceptable to describe compact systems, and we successfully compared the effects of all the necessary physical requirements with the standard results of f (G)-gravity, which can be retrieved at χ = 0.
1 Introduction The current phenomenon of accelerating cosmic expansion reveals the impressive evolution in modern physics. This phenomenon has prompted many researchers to explore the motif of this wonderful change in cosmic history. This prodigious change is contemplated as the outcome of a cryptical force dubbed as dark energy which covers about 68.3% of overall energy in the universe and possesses large negative pressure with repulsive nature; however, its remarkable highlights are not completely known. To investigate the puzzling attributes of this mysterious
a e-mail: [email protected] (corresponding author) b e-mail: [email protected] c e-mail: [email protected] d e-mail: [email protected]
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form of energy, there are mostly two ways to deal with puzzling source causing this cosmic accelerating expansion. The first way is to adjust the matter part to produce dynamic dark
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