We derive a working model for the TolmanOppenheimer-Volkoff equation for quark star systems within the modified f (T, T )-gravity class of models. We consider f (T, T )-gravity for a static spherically symmetric spacetime. In this instance the metric is built from a more fundamental tetrad vierbein from which the metric tensor can be derived. We impose a linear f (T ) parameter, namely taking f = αT (r ) + βT (r ) + ϕ and investigate the behaviour of a linear energy-momentum tensor trace, T . We also outline the restrictions which modified f (T, T )-gravity imposes upon the coupling parameters. Finally we incorporate the MIT bag model in order to derive the mass-radius and mass-central density relations of the quark star within f (T, T )-gravity.
We derive a Tolman-Oppenheimer-Volkoff equation in neutron star systems within the modified f (T, T ) -gravity class of models using a perturbative approach. In our approach f (T, T )-gravity is considered to be a static spherically symmetric space-time. In this instance the metric is built from a more fundamental vierbein which can be used to relate inertial and global coordinates. A linear func-is taken as the Lagrangian density for the gravitational action. Finally we impose the polytropic equation of state of neutron star upon the derived equations in order to derive the mass profile and mass-central density relations of the neutron star in f (T, T )-gravity.
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