Junction conditions in perfect fluid $f(\mathcal{G},~T)$ gravitational theory

TL;DR

This paper derives the junction conditions for smooth matching of spacetimes in $f( ext{Gauss-Bonnet}, T)$ gravity, showing that thin-shells are generally not allowed, thus constraining models like gravastars and wormholes.

Contribution

It provides the first complete set of junction conditions in $f( ext{Gauss-Bonnet}, T)$ gravity, including a scalar-tensor equivalence, and shows that thin-shells are not permissible in this theory.

Findings

Thin-shells are not allowed in the general $f( ext{Gauss-Bonnet}, T)$ gravity.

Complete junction conditions for smooth matching are established.

Scalar-tensor representation confirms the equivalence and results.

Abstract

This manuscript aims to establish the gravitational junction conditions(JCs) for the $f(\mathcal{G},~T)$ gravity. In this gravitational theory, $f$ is an arbitrary function of Gauss-Bonnet invariant $\mathcal{G}$ and the trace of the energy-momentum tensor $T_{\mu\nu}$ i.e., $T$. We start by introducing this gravity theory in its usual geometrical representation and posteriorly obtain a dynamically equivalent scalar-tensor demonstration on which the arbitrary dependence on the generic function $f$ in both $\mathcal G$ and $T$ is exchanged by two scalar fields and scalar potential. We then derive the JCs for matching between two different space-times across a separation hyper-surface $\Sigma$, assuming the matter sector to be described by an isotropic perfect fluid configuration. We take the general approach assuming the possibility of a thin-shell arising at $\Sigma$ between the two space-times. However, our results establish that, for the distribution formalism to be well-defined, thin-shells are not allowed to emerge in the general version of this theory. We thus obtain instead a complete set of JCs for a smooth matching at $\Sigma$ under the same conditions. The same results are then obtained in the scalar-tensor representation of the theory, thus emphasizing the equivalence between these two representations. Our results significantly constrain the possibility of developing models for alternative compact structures supported by thin-shells in $f(\mathcal{G},~T)$ gravity, e.g. gravastars and thin-shell wormholes, but provide a suitable framework for the search of models presenting a smooth matching at their surface, from which perfect fluid stars are possible examples.