Eur. Phys. J. Plus (2022) 137: 640
https://doi.org/10.1140/epjp/s13360-022-02850-0

Regular Article

Self-gravitating anisotropic compact objects in 5D EGB gravity

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, 411023, Khadakwasla, Pune, 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

^a sunil@unizwa.edu.om

Received: 22 February 2022
Accepted: 18 May 2022
Published online: 30 May 2022

Abstract

In this article, we investigate an anisotropic solution for compact static spherically symmetric objects as an alternative to neutron stars, which is a class of compact stars dubbed as strange stars in the context of five-dimensional Einstein–Gauss–Bonnet (EGB) theory by exploiting Tolman’s metric. With current sensitivities, we also consider a nonlinear equation of state along with an anisotropic source of matter which formed the basis for generating the bounded compact stars. The unknown constants are determined via the boundary conditions along with the Boulware–Deser geometry to describe as an exterior space-time. Observational mass data of the recently discovered millisecond pulsars, viz., PRS J1614-2230, PRS J1903+327, and LMC X-4, were used to predict radii via M–R curve which are lying in the range of . Furthermore, we discuss the stability of the model via adiabatic index and mass versus central mass density () profile. We find that a fine-tuning of the parameters coming from the theory, eventually, influences the inner geometry of compact stars and, therefore, influences important physical properties of realizable stellar structures. Moreover, the effects of EoS parameters on the mass and Bag constant are shown by the equi-plane diagrams. Conclusively, the results have shown that our stellar model is stable, physically acceptable, as well as it provides circumstantial evidence in favor of super-massive pulsars such as ultra-dense hypothetical strange stars in the background of five-dimensional EGB gravity.