Anisotropic Strange Star Model Beyond Standard Maximum Mass Limit by Gravitational Decoupling in $f(Q)$ Gravity

We study a class of static spherically symmetric vacuum solutions in modified teleparallel gravity solving the field equations for a specific model Ansatz, requiring the torsion scalar T to be constant. We discuss the models falling in this class. After some general considerations, we provide and investigate local solutions in the form of black holes and traversable wormholes as well as configurations that can match the anomalous rotation curves of galaxies.

Section: Introductionmentioning

confidence: 99%

A class of static spherically symmetric solutions in f(T)-gravity

Calzá,

Sebastiani

2024

“…Moreover, SSS geometries may also take into account another well-studied problem in experimental physics: the anomalous rotation of spiral galaxies. In those respect, SSS local solutions have been already explored in f (R)-gravity [52][53][54][55][56], in f (T )-gravity [57][58][59][60][61][62] and lately also in f (Q)-gravity [63][64][65][66][67][68][69][70][71][72][73][74][75][76].…”

Section: Introductionmentioning

confidence: 99%

A class of static spherically symmetric solutions in f(Q)-gravity

Calzà

Sebastiani

2023

“…From the perspective of the Friedmann-Laîmatre-Robertson-Walker (FLRW) evolution history, Gadbail et al [11] propose a number of fascinating explicit reconstructions for f (Q) gravity. In the context of f (Q) gravity, Maurya et al [12] have studied the gravitationally decoupled anisotropic solutions for strange stars by combining the Massachusetts Institute of Technology (MIT) bag model equation of state for hadronic matter with the Tolman metric ansatz. Lymperis [13] investigated the cosmic implications in f (Q) gravity, motivated by the interesting characteristics and a recently proposed general form of the function of nonmetricity scalar Q.…”

Section: Introductionmentioning

confidence: 99%

Physical properties of a quintessence anisotropic stellar model in f(Q) gravity and the mass–radius relation

Bhar

2023

In this article, we present a new family of solutions to the Einstein field equations of an uncharged spherically symmetric anisotropic matter distribution in the context of f(Q) gravity by choosing $$f(Q)=Q+aQ^2$$ f ( Q ) = Q + a Q 2 , a being the coupling constant. Along with the fundamental quintessence dark energy defined by the equation of state parameter $$-1<\omega _q<-\frac{1}{3}$$ - 1 < ω q < - 1 3 , we have generated the field equations in modified gravity. Using the linear relationship between radial pressure and energy density along with the Krori–Barua (KB) metric potential, we are able to solve the field equations. Next, we discuss the smooth matching between the exterior Schwarzschild spacetime and the interior spherically symmetric spacetime. We have presented a thorough physical analysis of several factors analytically and graphically to show the physical viability of our suggested model. For the compact star SAXJ 1808.4-3658, our entire graphical analysis was carried out in the context of our solutions for various values of the coupling constant connection to the f(Q) gravity. The influence of coupling constant “a” on different model parameters has been numerically determined and is presented in tabular form. We checked the radial and tangential sound speeds, the stability factor, the adiabatic index, etc. to determine whether our model was stable. It is evident from our analysis that the model is potentially stable when coupling constant $$a \in [0,\,5]$$ a ∈ [ 0 , 5 ] . The maximum allowable mass and radius from our present model have been obtained through the mass–radius ($$M-R$$ M - R ) plot for different values of a.