Abstract
An alternative gravity theory that has attracted considerable attention recently is the novel four-dimensional Einstein–Gauss–Bonnet (4EGB) gravity. This idea was proposed to bypass the Lovelock’s theorem and to permit nontrivial higher curvature effects on the four-dimensional local gravity. In this approach, the Gauss–Bonnet (GB) coupling constant alpha is rescaled by a factor of alpha /(D -4) in D dimensions and taking the limit D rightarrow 4. In this article, we analyze the effects of charge on static compact stars in the regularized 4D EGB gravity theory. Two classes of new exact solutions are found for a particular choice of the gravitational potential and assuming a relationship between the electric field intensity and the spatial potential. A graphical analysis indicates that the matter and electromagnetic variables are well behaved for specific values of the parameter space. Finally, based on physical grounds appropriate bounds on the model parameters we show that compact objects with the value of adiabatic index gamma is consistent with expectations.
Highlights
EGB gravity involves the second order Lovelock polynomial terms, appears in the low energy effective action of heterotic string theory [4] and leads to ghost-free nontrivial gravitational self-interactions [5]
Page 11 of 12 790 constant could contribute to the Einstein’s field equations by introducing a redefinition α → α/(D − 4) in D dimension and taking the limit D → 4. Motivated by this gravity theory, in this work, we thoroughly investigate static and spherically symmetric compact charged spheres made of a charged perfect fluid
After converting the master pressure isotropy equation we obtained an exact solution by prescribing an ansatz for the gravitational potential Z and by connecting the electric-field intensity E with Z to simplify the master field equation
Summary
EGB gravity involves the second order Lovelock polynomial terms, appears in the low energy effective action of heterotic string theory [4] and leads to ghost-free nontrivial gravitational self-interactions [5] For these reasons the role of the GB contribution has been actively studied in recent times. Extending this work we would like to develop exact solutions that may be used to describe the dynamics of charged compact objects in strong gravitational fields such as is applicable to neutron/quark stars (NS/QS). In order to see any appreciable effect on the phenomenology of the compact stars, several efforts have been made starting from Bekenstein [51] He generalized the Tolman–Oppenheimer–Volkoff (TOV) equations of hydrostatic equilibrium to the charged case, and discussed their applicability.
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