Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Abstract

In this current study, our main focus is on modeling the specific charged compact star SAX J 1808.4-3658 (M = 0.88 $$M_{\odot }$$ M ⊙ , R = 8.9 km) within the framework of $$f(R,\,T)$$ f ( R , T ) modified gravity theory using the metric potentials proposed by Tolman–Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner–Nordström line element at the surface of the star. Tolman–Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve the Einstein–Maxwell field equations where the density profile ($$\rho $$ ρ ) is related to the radial pressure ($$p_{\mathrm{r}}$$ p r ) as $$p_{\mathrm{r}}(r) = (\rho - 4B_{\mathrm{g}})/3$$ p r ( r ) = ( ρ - 4 B g ) / 3 . Furthermore, to derive the values of the unknown constants $$a,\, b,\, B,\, C$$ a , b , B , C and the bag constant $$B_{\mathrm{g}}$$ B g , we match our interior spacetime to the exterior Reissner–Nordström line element at the surface of stellar system. In addition, to check the physical validity and stability of our suggested model we evaluate some important properties, such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which shows the viability of our present model in the context of $$f(R,\,T)$$ f ( R , T ) modified gravity.

Kuchowicz gravastars in the braneworld formalism

“…In the end, we came to the conclusion that we have derived new, non-singular and horizonless gravastar model for braneworld gravity with the impact of Kuchowicz metric potential. Generally, with special metric potential it is more challenging to obtain physically acceptable solutions, but, as one could notice, interest to the Tolman-Kuchowicz metric potentials for the compact objects (exotic stars for example) have grown in this decade (see [37][38][39][40][41][42]), and thus it is important to test the Kuchowicz spacetime on static gravastars.…”

Dark Energy Stars in Tolman-Kuchowicz spacetime in the context of Einstein Gravity

“…On the other hand, in the context of modified gravity, we now discuss the uses of TK metric potentials. Bhar et al [47] had previously employed this metric potential to model compact objects in Einstein Gauss Bonnet gravity and Javed et al [48] used this metric potential to model anisotropic spheres in f (R, G) modified gravity, Majid and Sharif [49] obtained quark stars in massive Brans-Dicke gravity, Biswas et al [50] obtained an anisotropic strange star with f (R, T ) gravity, Farasat Shamir and Fayyaz [51] obtained the model of charged compact star in f (R) gravity, Naz and Shamir [52] found the stellar model in f (G) gravity, Rej et al [53] studied the charged compact star in the context of f (R, T ) gravity. One notices that TK metric potential succeed in producing the model of a compact star that lacks singularity and meets all the physically acceptable requirements.…”

Model of hybrid star with baryonic and strange quark matter in Tolman-Kuchowicz spacetime

“…However, we will now consider the application of this metric potential in the context of modified gravity. Earlier, Bhar et al [109] used this metric potential to model compact objects in Einstein-Gauss-Bonnet gravity, Javed et al [110] used it to model anisotropic spheres in f (R, G) modified gravity, Biswas et al [111] obtained an anisotropic strange star with f (R, T ) gravity, Majid and Sharif [112] obtained quark stars in massive Brans-Dicke gravity, Naz and Shamir [113] discovered the stellar model in f (G) gravity, Farasat Shamir and Fayyaz [114] discovered the model of charged compact star in f (R) gravity, Rej et al [115] investigated the charged compact star in f (R, T ) gravity, Bhar et al [116] studied anisotropic compact star in Rastall gravity. It's worth noting that this metric potential successfully produces a compact stellar model that is singularity-free and meets all of the physical requirements.…”

“…Several authors have successfully employed the TK ansatz to develop a realistic and stable model of compact stars, both in the context of General Relativity and of alternative theories of gravity, and it will be explored in detail in the next sections. Recently, we have modelled a charged compact star in f (R, T ) gravity by using the TK metric [98]. In the present work, we have developed a hybrid star model constituted with SQM and normal baryonic matter in Einstein gravity, employing two types of EoSs; a simple linear relation between the radial pressure and the matter density for barynoic matter and a well-established phenomenological MIT bag model EoS in the well-studied TK ansatz background for SQM.…”