  Convection and turbulence in core-collapse supernovae (CCSNe) are inherently
three-dimensional in nature. However, 3D simulations of CCSNe are
computationally demanding. Thus, it is valuable to modify simulations in
spherical symmetry to incorporate 3D effects using some parametric model. In
this paper, we report on the formulation and implementation of general
relativistic (GR) neutrino-driven turbulent convection in the spherically
symmetric core-collapse supernova code \texttt{GR1D}. This is based upon the
recently proposed method of Supernova Turbulence in Reduced-dimensionality
(\textit{STIR}) in Newtonian simulations from \cite{Couch2020_STIR}. When the
parameters of this model are calibrated to 3D simulations, we find that our GR
formulation of \textit{STIR} requires larger turbulent eddies to achieve a
shock evolution similar to the original \textit{STIR} model. We also find that
general relativity may alter the correspondence between progenitor mass and
successful vs.~failed explosions.
