A Perturbative Approach to Neutron Stars in $f(T, \mathcal{T})-$Gravity

Understand

We derive a Tolman-Oppenheimer-Volkoff equation in neutron star systems within the modified $f(T, \mathcal{T})$-gravity class of models using a perturbative approach.

• In our approach $f(T, \mathcal{T})$-gravity is considered to be a static spherically symmetric space-time.
• In this instance the metric is built from a more fundamental tetrad vierbein which can be used to relate inertial and global coordinates.
• A linear function $f = T(r) + \mathcal{T}(r) + \chi h(T, \mathcal{T}) + \mathcal{O}(\chi^{2})$ is taken as the Lagrangian density for the gravitational action.