General Relativistic Neutrino-Driven Turbulence in One-Dimensional Core-Collapse Supernovae

TL;DR

This paper develops a general relativistic model for neutrino-driven turbulence in spherically symmetric core-collapse supernova simulations, aiming to incorporate 3D effects efficiently and explore GR's impact on explosion outcomes.

Contribution

It formulates and implements a GR version of the STIR turbulence model in 1D supernova simulations, extending previous Newtonian approaches to include relativistic effects.

Findings

GR turbulence model requires larger eddies for similar shock evolution

GR effects may influence the relation between progenitor mass and explosion success

Calibration to 3D simulations enhances model accuracy

Abstract

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.