arXiv:2412.03659v1 Announce Type: new
Abstract: Many astrophysical systems of interest to numerical relativity, such as rapidly rotating stars, black hole accretion disks, and core-collapse supernovae, exhibit near-symmetries. These systems generally consist of a strongly gravitating central object surrounded by an accretion disk, debris, and ejecta. Simulations can efficiently exploit the near-axisymmetry of these systems by reducing the number of points in the angular direction around the near-symmetry axis, enabling efficient simulations over seconds-long timescales with minimal computational expense. In this paper, we introduce GRoovy, a novel code capable of modeling astrophysical systems containing compact objects by solving the equations of general relativistic hydrodynamics (GRHD) in full general relativity using singular curvilinear (spherical-like and cylindrical-like) and Cartesian coordinates. We demonstrate the code’s robustness through a battery of challenging GRHD tests, ranging from flat, static spacetimes to curved, dynamical spacetimes. These tests further showcase the code’s capabilities in modeling systems with realistic, finite-temperature equations of state and neutrino cooling via a leakage scheme. GRoovy extensively leverages GRHayL, an open-source, modular, and infrastructure-agnostic general relativistic magnetohydrodynamics library built from the highly robust algorithms of IllinoisGRMHD. Long-term simulations of binary neutron star and black hole-neutron star post-merger remnants will benefit greatly from GRoovy to study phenomena such as remnant stability, gamma-ray bursts, and nucleosynthesis.
Future Roadmap
GRoovy, a novel code for modeling astrophysical systems in numerical relativity, shows great promise in its ability to efficiently simulate systems with near-symmetries. Moving forward, there are several potential challenges and opportunities on the horizon.
Challenges
- Computational Expense: Despite the efficiency of GRoovy, simulations of long-term phenomena such as binary neutron star and black hole-neutron star post-merger remnants will still require significant computational resources. Finding ways to optimize the code further and utilize parallel computing architectures will be crucial.
- Complex Equations of State: Modeling systems with realistic, finite-temperature equations of state presents a challenge. GRoovy’s ability to handle such equations is a major advantage, but there is still room for improvement and refinement.
- Accuracy and Robustness: While GRoovy has shown robustness in its performance on a battery of GRHD tests, ongoing validation and verification efforts will be necessary to ensure its accuracy in capturing the physics of astrophysical systems.
Opportunities
- Remnant Stability: GRoovy can be utilized for long-term simulations to study the stability of binary neutron star and black hole-neutron star post-merger remnants. This investigation can provide valuable insights into the behavior and evolution of these systems.
- Gamma-Ray Bursts: By studying the post-merger remnants with GRoovy, researchers can investigate the conditions necessary for the production of gamma-ray bursts. Understanding these energetic events can shed light on the physics of high-energy astrophysical phenomena.
- Nucleosynthesis: GRoovy’s capabilities can also contribute to the study of nucleosynthesis, the process through which elements are formed in astrophysical environments. By simulating the remnants, researchers can gain insights into the nuclear reactions and abundances that occur.
Overall, the development and utilization of GRoovy can significantly enhance our understanding of astrophysical systems with compact objects. By addressing the challenges and seizing the opportunities ahead, this code has the potential to unlock new discoveries in the field of numerical relativity.