Astronomical observations have confirmed that the heavy elements in the universe were synthesized in stars and stellar explosions, yet many questions concerning how and where these elements formed remain outside the purview of direct observation. Through the ExaStar multiphysics codes, exascale computing will be used to simulate supernova explosions and neutron star mergers, addressing fundamental questions in astrophysics, such as the origin of elements, the physics of ultra-dense matter, and the sources of gravitational waves.

Project Details

ExaStar focuses on developing a new component-based multiphysics code suite with adaptive mesh refinement (AMR) that can accurately simulate coupled hydrodynamics, radiation transport, thermonuclear kinetics, and nuclear microphysics for stellar explosion simulations. The code will reach exascale efficiency by building upon current multicore and many-core efficient local physics packages integrated into a task-based asynchronous execution framework by using current AMR technology. The fundamental goal is to understand the production of the heavier chemical elements produced and expelled in explosions, such a supernovae and neutron star mergers.

Although astronomical observations reveal that the production of the heaviest nuclei began early in galactic history, it is unknown exactly how and where these elements were formed. To address this topic via laboratory measurements, a series of nuclear science long-range plans have supported the construction of radioactive ion beam facilities, culminating in the Facility for Rare Isotope Beams (FRIB). Although FRIB is designed to acquire extensive data on the nuclei relevant for astrophysical nucleosynthesis, its end science goal cannot be met unless those experimental data are integrated into high-fidelity simulations of stellar explosions, such as supernovae and neutron star mergers, that define the conditions under which such heavy element production occurs. Through a better understanding of the sites in which the heaviest elements are made, ExaStar can help focus experimental efforts at FRIB on the reactions of greatest influence.

Simulating stellar explosions represents a quintessential multiphysics challenge. The hydrodynamics of the astrophysical gas must include a specialized equation of state, capturing the behavior of matter at extreme density. The impact of gravity should ideally be treated by solving Einstein’s equations of general relativity. Accurately calculating the radiation transport of neutrinos is crucial for driving the explosion shockwave and setting the neutron-to-proton ratio that determines the nucleosynthetic yields. To determine those yields, in situ nuclear kinetics with ideally thousands of isotopes must follow the complex flow of reactions. Finally, predicting the observable signals of the event (i.e., photons, neutrinos, and gravitational waves) requires the simulation to be postprocessed with multi-angle spectral radiation transport.

The ExaStar base challenge problem is a 3D simulation of the explosion of a massive star in a core-collapse supernova. The initial conditions will be taken from stellar evolution models of a late-stage star at the point of iron core collapse. The physical domain of the simulation will enclose the helium shell of the star, which has a radius around 10,000 km, with a maximum spatial resolution enabled by AMR that is finer than 1 km in the innermost regions. At least 20 energy groups will be used to resolve the spectra of neutrinos of all flavors (i.e., electron, mu, tau, and their antiparticles) from 0 to 300 MeV. A detailed set of tabulated neutrino-matter interaction rates will be used to model emission, absorption, scattering, and pair production processes and will be integrated with a high-density equation of state that provides pressures, entropies, and other thermodynamic variables. A Newtonian multi-pole solver will be available to simulate gravity with the potential to upgrade this with a full general relativistic dynamical space-time solver.

In Figure 1, Hot material roils around a newly-born neutron star at the center of a core-collapse supernova. Shown is the matter entropy from a three-dimensional simulation of the first half second of the explosion. Driven by intense heating from neutrinos coming from the cooling neutron star at the center, the shock wave will be driven outward, eventually ripping the star apart and flinging the elements that make up our solar system and ourselves into interstellar space.

Exastar 3D simulation of core-collapse supernova

Figure 1: ExaStar 3D simulation of a Core-collapse supernova performed using the ORNL Chimera multiphysics code

Principal Investigator(s):

Daniel Kasen, Lawrence Berkeley National Laboratory


Lawrence Berkeley National Laboratory, Oak Ridge National Laboratory, Argonne National Laboratory, State University of New York at Stony Brook, Michigan State University

Progress to date

  • A new neutrino transport module was developed by using Discontinuous Galerkin methods. Also, the transport was coupled to a hydrodynamics solver, and the accuracy was verified.
  • A dynamical spacetime solver was developed that solves Einstein’s equations of general relativity, and the solver was exercised on a simulation of two merging black holes.
  • GPU implementations of nearly all multiphysics modules were completed, including neutrino transport, general relativistic gravity, nuclear kinetics, hydrodynamics, and a nonpolytropic equation of state. On-node performance was also profiled.
  • Adaptive meshing was integrated from AMReX into the Flash multiphysics code, and baseline calculations were performed on Summit.

By using exascale computing to model the physics of stellar explosions, ExaStar will inform planned and future astrophysical experimental observations to answer questions about the origin of heavy nuclides in the universe.

National Nuclear Security Administration logo U.S. Department of Energy Office of Science logo