Bardeen stellar structures with Karmarkar condition

Abstract

This current study is focussed to discuss the existence of a new family of compact star solutions by adopting the Karmarkar condition in the background of Bardeen black hole geometry. For this purpose, we consider static spherically symmetric spacetime with anisotropic fluid distribution in the presence of electric charge. We consider a specific model of grr metric function, to describe a new family of solutions which satisfies the Karmarkar condition. Further, we investigate the interior solutions for two different models of compact stars with observational mass and radii, i.e., (M = 1.77M⊙, R b = 9.56km) and (M = 1.97M⊙, R b = 10.3km). It is found that these solutions fulfill all the necessary conditions for a charged star. Through graphical discussion, it is noticed that our calculated solutions are physically arguable with a best degree of accuracy for n ∈ [1.8, 7), where parameter n is involved in the model under discussion. However, it is perceived that the presented model violates all the physical conditions for n ∈ {2, 4, 6}. Finally, it is concluded that the parameter n has a strong impact on the obtained solutions in the context of Bardeen stellar structures.

Physical Attributes of Bardeen Stellar Structures in f R Gravity

“…Thus, the repulsive nature of anisotropy confirms the physically acceptable behavior of the chosen stars (iv) Figure 6 shows that all the energy constraints are fulfilled (v) Figure 7 represents the balancing behavior of (F g ), (F h ), (F a ), and (F e ) forces for our proposed viable f ðRÞ gravity model (vi) For the well-behaved nature of the compact objects, the graphical response of EoS must fulfill the condition 0 < w r and w t < 1: The corresponding plots given in Figure 8 show the consistent behavior of our proposed model of the f ðRÞ gravity (vii) For stellar objects, the values of velocity of sounds v 2 r for r and v 2 t for t should be furnished within limits of ½0, 1: It is clear from Figure 11 that the causality constraints exhibit satisfactory nature for considered stellar structure. Furthermore, the Abreu approach outcomes are also consistent for the considered f ðRÞ gravity model (viii) It has been noted from Figure 9 that the plots of MðrÞ and UðrÞ exhibit monotonically increasing nature while the plot of ZðrÞ is monotonically decreasing; this implies that we establish a stable system (ix) The radial and transverse adiabatic index values denoted by γ r and γ t for the chosen model are greater than 4/3, as shown in Figure 10, which confirms the stability of our system Thus, our presented work satisfied all those results proposed by Mustafa et al [83] under the frame of GR. This confirms that our considered f ðRÞ gravity model is entirely stable and physically acceptable.…”

“…The term q denotes charge within the core of compact objects corresponding to r. Furthermore, the expression for electric field can be considered as E 2 = kQr [83] and E 2 = F 10 F 01 , which is expressed as E 2 = q 2 /r 4 : The f ðRÞ field equations for (3) are given as…”

“…In addition, the charged stellar structure along with the Bardeen sphere in the background of conformal motion was explored [82]. In a recent paper [83], compact star solutions have been discussed for the Bardeen sphere by using the famous Karmarkar approach. Being motivated from the above literature, here, we explore the studies of Mustafa et al [83] in the context of modified f ðRÞ theory by assuming the charged compact structures along with the Bardeen model.…”

“…In particular, we study the physical attributes of the compact objects against various values of M for different ranges of R, i.e., R = 10:10 km with M = 1:2,1:3,1:4,1:5ðM e Þ, R = 9:10 km with M = 1:2,1:4ðM e Þ, and R = 8:10 km with M = 1:2ðM e Þ. For this purpose, we take specific electric fields E 2 = kQr [83] and establish physically appropriate models of compact stars.…”

Anisotropic Strange Star in 5D Einstein-Gauss-Bonnet Gravity

“…In this section, we will discuss the anisotropic solution in 5D Einstein-Gauss-Bonnet (EGB) gravity. Recently, some pinioning works on anisotropy on the compact star models have been widely discussed in classical general relativity and modified gravity theory by several authors [60][61][62][63][64][65][66][67][68][69][70][71][72][73][74]. Here, our aim is to generate an exact solution of the system of Equations ( 9)-( 11) for anisotropic matter distribution.…”