A New Open-Source Code for Spherically-Symmetric Stellar Collapse to Neutron Stars and Black Holes

TL;DR

This paper introduces GR1D, an open-source spherically-symmetric GR hydrodynamics code for simulating stellar collapse to neutron stars and black holes, incorporating microphysics, neutrino schemes, and rotation effects.

Contribution

The paper presents a new open-source 1D GR hydrodynamics code with microphysical EOS, neutrino leakage, and rotation, enabling detailed stellar collapse simulations and black hole formation studies.

Findings

Good agreement with full Boltzmann neutrino simulations on black hole formation timing.

Demonstrated capability to model rotating core-collapse supernovae.

Validated the code with standard test calculations.

Abstract

We present the new open-source spherically-symmetric general-relativistic (GR) hydrodynamics code GR1D. It is based on the Eulerian formulation of GR hydrodynamics (GRHD) put forth by Romero-Ibanez-Gourgoulhon and employs radial-gauge, polar-slicing coordinates in which the 3+1 equations simplify substantially. We discretize the GRHD equations with a finite-volume scheme, employing piecewise-parabolic reconstruction and an approximate Riemann solver. GR1D is intended for the simulation of stellar collapse to neutron stars and black holes and will also serve as a testbed for modeling technology to be incorporated in multi-D GR codes. Its GRHD part is coupled to various finite-temperature microphysical equations of state in tabulated form that we make available with GR1D. An approximate deleptonization scheme for the collapse phase and a neutrino-leakage/heating scheme for the postbounce epoch are included and described. We also derive the equations for effective rotation in 1D and implement them in GR1D. We present an array of standard test calculations and also show how simple analytic equations of state in combination with presupernova models from stellar evolutionary calculations can be used to study qualitative aspects of black hole formation in failing rotating core-collapse supernovae. In addition, we present a simulation with microphysical EOS and neutrino leakage/heating of a failing core-collapse supernova and black hole formation in a presupernova model of a 40 solar mass zero-age main-sequence star. We find good agreement on the time of black hole formation (within 20%) and last stable protoneutron star mass (within 10%) with predictions from simulations with full Boltzmann neutrino radiation hydrodynamics.