Charged anisotropic strange stars in f ( G ) $f(\mathcal{G})$ gravity
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ORIGINAL ARTICLE
Charged anisotropic strange stars in f (G) gravity M. Sharif1 · Amna Ramzan1
Received: 16 June 2020 / Accepted: 3 August 2020 © Springer Nature B.V. 2020
Abstract This paper examines the charged anisotropic strange stars by employing the embedding class-1 condition in the framework of f (G) gravity. For this reason, we use MIT bag model to derive the expression of charge inside the geometry. We evaluate the unknown constants by the matching of interior spacetime with the Riessner-Nordström geometry. The radii are predicted for the star models like Vela X-1, 4U 1608-52, LMC X-4 and PSR J0348+0432 by using their observed masses. We check the viability and stability of the resulting solution through graphical behavior of matter components, energy constraints, adiabatic index and causality condition. It is observed that strange stars exhibit more dense behavior in the presence of charge and MIT bag model. We conclude that embedding class-1 solution shows viable and stable behavior for charged anisotropic strange stars in this theory. Keywords Anisotropy · f (G) theory · Strange stars
1 Introduction Among the plethora of mysterious constituents of the universe, stars are identified as basic components of our galaxy. The fusion reaction in the core of a star produces the outward directed thermal pressure which is balanced by the inward directed force of gravity to hold the star in equilibrium state. When the fuel in a star is burnt out completely,
B M. Sharif
[email protected] A. Ramzan [email protected]
1
Department of Mathematics, University of the Punjab, Quaid-e-Azam Campus, Lahore-54590, Pakistan
the inward directed gravitational force overcomes the outward directed pressure, hence the star undergoes its stellar death, referred to as gravitational collapse. As a result, compact objects are formed that are categorized as less massive white dwarfs and more massive neutron stars as well as black holes. Among these stellar structures, neutron stars have attracted the observers to discuss their composition, structure and features. The less dense core of neutron star provides the chance to change it into quark stars or strange stars. Compact structures which are highly dense and made of strange, up and down quarks are known as strange stars or quark stars. This hypothetical compact object compels many researchers to study their interior formation (Witten 1984; Alcock et al. 1986; Haensel et al. 1986; Li et al. 1995 and Drago et al. 1996). It is observed that the existence of anisotropy in spherically symmetric objects induces important physical characteristics of celestial bodies. Ruderman (1972) proposed that nuclear matter possesses anisotropy if the matter density for relativistic object is equal to 1015 g/cm3 . Herrera and Santos (1997) analyzed the causes and effects of local anisotropy in self-gravitating systems by considering both Newtonian and general relativistic examples. Harko and Mak (2002) investigated the solution for anisotropic objects and analyzed their physical feat
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