Simulating the Cosmic Dawn With Enzo

@article{Norman2018SimulatingTC,
  title={Simulating the Cosmic Dawn With Enzo},
  author={Michael L. Norman and Britton D. Smith and James Bordner},
  journal={Frontiers in Astronomy and Space Sciences},
  year={2018}
}
We review two decades of progress using the Enzo hydrodynamic cosmology code to simulate the Cosmic Dawn, a period of roughly 1 billion years beginning with the formation of the first stars in the universe, and ending with cosmic reionization. Using simulations of increasing size and complexity, working up in length and mass scale and to lower redshifts, a connected narrative is built up covering the entire epoch. In the first part of the paper, we draw on results we and our collaborators have… 
2 Citations
Makemake + Sedna: A Continuum Radiation Transport and Photoionization Framework for Astrophysical Newtonian Fluid Dynamics
Astrophysical fluid flow studies often encompass a wide range of physical processes to account for the complexity of the system under consideration. In addition to gravity, a proper treatment of
Nyx: A Massively Parallel AMR Code for Computational Cosmology
We present a new N-body and gas dynamics code, called Nyx, for large-scale cosmological simulations. Nyx follows the temporal evolution of a system of discrete dark matter particles gravitationally

References

SHOWING 1-10 OF 200 REFERENCES
Computer Simulations of Cosmic Reionization
The cosmic reionization of hydrogen was the last major phase transition in the evolution of the universe, which drastically changed the ionization and thermal conditions in the cosmic gas. To the
SIMULATIONS ON A MOVING MESH: THE CLUSTERED FORMATION OF POPULATION III PROTOSTARS
The cosmic dark ages ended a few hundred million years after the big bang, when the first stars began to fill the universe with new light. It has generally been argued that these stars formed in
Dark-ages Reionization and Galaxy formation simulation – I. The dynamical lives of high-redshift galaxies
We present the Dark-ages Reionization and Galaxy-formation Observables from Numerical Simulations (DRAGONS) program and Tiamat, the collisionless N-body simulation program upon which DRAGONS is
Early structure formation in quintessence models and its implications for cosmic reionization from first stars
We present the first hydrodynamic N-body simulations of primordial gas clouds responsible for the reionisation process in dark energy cosmologies. We compare the cosmological constant scenario with a
Simulations of Pregalactic Structure Formation with Radiative Feedback
We present results from three-dimensional hydrodynamic simulations of the high-redshift collapse of pregalactic clouds including feedback eUects from a soft photodissociating UV radiation —eld. The H
The first stars: formation of binaries and small multiple systems
We investigate the formation of metal-free, Population III (Pop III), stars within a minihalo at z ~ 20 with a smoothed particle hydrodynamics (SPH) simulation, starting from cosmological initial
The first miniquasar
We investigate the environmental impact of the first active galactic nuclei that may have formed ∼150 Myr after the big bang in low-mass ∼10 6 M θ minihaloes. Using ENZO, an adaptive-mesh refinement
How Very Massive Metal-Free Stars Start Cosmological Reionization
The initial conditions and relevant physics for the formation of the earliest galaxies are well specified in the concordance cosmology. Using ab initio cosmological Eulerian adaptive mesh refinement
The Transition from the First Stars to the Second Stars in the Early Universe
We observe a sharp transition from a singular, high-mass mode of star formation to a low-mass-dominated mode, in numerical simulations, at a metallicity of 10-3 Z☉. We incorporate a new method for
Constraints on the IMF of the first stars
Motivated by theoretical predictions that first stars were predominantly very massive, we investigate the physics of the transition from an early epoch dominated by massive Pop III stars to a later
...
...