Abstract
In the present article, we have presented completely new exact, finite and regular class I solutions of Einstein’s field equations i.e. the solutions satisfy the Karmarkar condition. For this purpose needfully we have introduced a completely new suitable g_{rr} metric potential to generate the model. We have investigated the various physical aspects for our model such as energy density, pressure, anisotropy, energy conditions, equilibrium, stability, mass, surface and gravitational red-shifts, compactness parameter and their graphical representations. All these physical aspects have ensured that our proposed solutions are well-behaved and hence represent physically acceptable models for anisotropic fluid spheres. The models have satisfied causality and energy conditions. The presented models are also stable by satisfying Bondi condition and Abreu et al. condition, in equilibrium position and static by satisfying TOV equation, Harrison–Zeldovich–Novikov condition, respectively. For the parameters chosen in the paper are matching in modeling Vela X-1, Cen X-3, EXO 1785-248 and LMC X-4. The M–R graph generated from the solutions is matching the ranges of masses and radii for the considered compact stars. This work also estimated the approximate moment of inertia for the mentioned compact stars.
Highlights
Many researchers are interested to investigate the properties of compact stars in higher dimensions
Liddle et al [13] have analyzed the effect of extra dimensions in the maximum mass of neutron stars (NS)
They have assumed an equation of state for non-interacting cold neutrons and found that the maximum mass of NS was reduces by the presence of extra dimensions
Summary
Many researchers are interested to investigate the properties of compact stars in higher dimensions. Karmarkar [20] embedded 4-dimensional spacetime into 5dimensional Euclidean space known as class I This method implies an equation that links the metric coefficients gtt and grr thereby simplifying to solve the field equations. Mak and Harko [22] derived the condition for lower limit of mass for any anisotropic compact stars which was strongly depends on degree of anisotropy. Dev and Gleiser [23] derived the critical condition for compactness parameter 2M/R for anisotropic relativistic stars and was found strongly depends on nature and degree of anisotropy. In this article we are exploring new physical solutions satisfying field equations under class I category and discuss the solutions to model compact stars.
Sign-in/Register to view highlights & summary 
Published Version (
Free)
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
