Anisotropic Quintessence Strange Stars in f(T) Gravity with Modified Chaplygin Gas

Abstract

In this paper, we study the existence of strange star in the background of ( ) modified gravity where is a scalar torsion. In KB metric space, we derive the equations of motion using anisotropic property within the spherically strange star with modified Chaplygin gas in the framework of modified ( ) gravity. Then we obtain many physical quantities to describe the physical status such as anisotropic behavior, energy conditions, and stability. By the matching condition, we calculate the unknown parameters to evaluate the numerical values of mass, surface redshift, etc., from our model to make comparison with the observational data. 2 Advances in High Energy Physics in ( ) gravity. Recently there are some static solutions which are spherically symmetric with charged source in ( ) theory [25]. The physical conditions have been studied [26] for the existence of astrophysical stars in ( ) theory after obtaining a large group of static perfect fluid solutions [27]. Capozziello et. al [ ] have shown that, instead of ( ) gravity, ( ) removes the singularities for the exact black hole solution in D-Dimensions. Wormhole solution has been studied under ( ) gravity by Sharif and Rani [ ]. ey have also investigated ( ) gravity for static wormhole solution to verify energy conditions [ ]. Again, for charged noncommutative wormhole solutions in f(T) gravity, Sharif and Rani [ , ] have seen that this solution exists by violating energy conditions.Generally, perfect fluid (isotropic fluid) inside the stellar object to study stellar structure and evolution is assumed because there exists isotropic pressure inside the fluid sphere. However, present observation shows that the fluid pressure of the highly compact astrophysical objects like X-ray pulsar, Her-X-, X-ray buster U -, millisecond pulsar SAXJ . -, etc. becomes anisotropy in nature which means the pressure can be rotten into two components such that one is radial pressure ( ) and the other is transverse pressure ( ). Now, Δ = − is known as the anisotropic factor. e anisotropy may arise for the different cases such as the existence of solid core, in presence of type P superfluid, phase transition, rotation, magnetic field, mixture of two fluids, and existence of external field. Generally, strange quark matter contains u, d, and s quarks. ere are two ways to classify the formation of strange matter [ ]. One way is the transformation of the quark hadron phase in the early universe and the other way is the reformation of neutron stars to strange matter at ultrahigh densities. A strange star is composed of the strange matter. Again the strange star can be classified into two types: Type I strange star with / > 0.3 and Type II strange star with 0.2 < / < 0.3. Depending on mass, radius, and energy density, the strange star is distinguished from the neutron star [ ]. It has been the most interesting topic to study the models of anisotropic stars for the last periods in GR and modified theories of gravity [35]. There have been many discussions about anisotropic star models in [36][37]...

Anisotropic compact objects in f(T) gravity with Finch–Skea geometry

“…The process reaches a stable configuration which is free from horizons and singularities. Recently Saha et al [46] studied anisotropic stellar models with interior space-time geometry described by Krori-Barua metric with modified Chaplygin gas in f (T ) gravity. Motivated by the above works, we also analyzed anisotropic compact stellar models with Finch-Skea geometry in f (T ) framework with modified Chaplygin gas (MCG).…”

On quintessence star model and strange star

“…The existence of these with the equations for the radial and tangential pressures given by (7) and (8) is a new theoretical proposal presented in this work., Its possible physical existence is justified by the astrophysics observations related to the accelerated expansion of the universe. In previous work stellar models with quintessence dark energy have already been approached [20][21][22][23]38] as well as proposals based on the MIT Bag model for strange stars [56][57][58][59][60]. One substantial difference in our case is the proposal of the equation of state (8), which can be understood as the consequence of the interaction between ordinary matter and the quintessence.…”

“…On the other hand there have been some approaches at a stellar level to describe compact objects [20][21][22][23], considering that the interior of the stars is formed by ordinary neutral matter [24][25][26][27][28][29][30], ordinary charged matter [31][32][33][34][35][36][37], and also by sources which are a combination of ordinary matter and quintessence dark energy, consistent with neutron stars [38]. Neutron or quark stars are not exclusively composed of neutrons or quarks, respectively, but rather these stars are formed predominantly by one of those particles.…”

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

“…Studies on anisotropic stars in different types of modified gravity theories are available in literature [41,[47][48][49][50][51]. Saha and Debnath [52] have investigated anisotropic stars in f (T) gravity with modified Chaplygin gas. The anisotropic compact stars with a quintessence field and modified Chaplygin gas in the framework of f (T) gravity model has been studied by Saha and Debnath [53].…”