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]...

In this work, we get an idea of the existence of compact stars in the background of f (T ) modified gravity where T is a scalar torsion. We acquire the equations of motion using anisotropic property within the spherically compact star with electromagnetic field, quintessence field and modified Chaplygin gas in the framework of modified f (T ) gravity. Then by matching condition, we derive the unknown constants of our model to obtain many physical quantities to give a sketch of its nature and also study anisotropic behavior, energy conditions and stability. Finally, we estimate the numerical values of mass, surface redshift etc from our model to compare with the observational data for different types of compact stars.

In this work, we study the existence of strange stars in the background of f(T,T) gravity in the Einstein spacetime geometry, where T is the torsion tensor and T is the trace of the energy-momentum tensor. The equations of motion are derived for anisotropic pressure within the spherically symmetric strange star. We explore the physical features like energy conditions, mass-radius relations, modified Tolman–Oppenheimer–Volkoff (TOV) equations, principal of causality, adiabatic index, redshift and stability analysis of our model. These features are realistic and appealing to further investigation of properties of compact objects in f(T,T) gravity as well as their observational signatures.

Abstract-In this paper, a compact, circularly polarized printed monopole antenna is proposed at ISM band (2.4-2.48 GHz) for biotelemetry and implantable applications. The proposed antenna possesses a small dimension (10 × 10 × 0.3 mm 3 ) and simple microstrip feeding structure. The circular polarization is easily achieved by introducing an "L" shape stub at the ground plane in ISM. The simulated 10 dB impedance bandwidth is around 13.87%, and 3 dB AR bandwidth is around 5.3%. The effect of different body phantoms is discussed to evaluate the sensitivity of the proposed antenna. The simulated peak gain of the proposed antenna is about −7.79 dBi across the operating band. The SAR analysis of the antenna configuration has also been studied.

Abstract-In this paper, a compact planar quasi-Yagi antenna with enhanced radiation characteristics is presented. The proposed structure is designed by incorporating metamaterial unit cells in place of conventional directors. Here, the technique used for directivity improvement is that the refractive index of the metamaterial is lower than that of the antenna substrate, which acts as a regular lens for beam focusing. Loading the quasi-Yagi antenna with metamaterial results in directivity as well as gain enhancement at the end-fire direction compared to the quasi-Yagi antenna with directors. In addition, reduction in the overall size of the proposed quasi-Yagi antenna by 26.67% is achieved. An enhanced impedance bandwidth has also been noticed. The gain performance of the proposed antenna within the frequency band has been studied.