Computational advances and challenges in simulations of turbulence and star formation

arXiv:2510.12203 · astro-ph.GA, astro-ph.IM, astro-ph.SR, physics.comp-ph, physics.flu-dyn · Submitted 2025-10-14 · Read on arXiv

astro-ph.GA, astro-ph.IM, astro-ph.SR, physics.comp-ph, physics.flu-dyn

Submitted: 2025-10-14

Updated: 2026-09-23

Code: https://github.com/pfhopkins/gizmo-public

Project page: https://princetonuniversity.github.io/Athena-Cversion

Terminology

• Core — 45× in this paper · explained in 2 episodes
• Accuracy — 30× in this paper · explained in 1 episode
• Monte Carlo — 20× in this paper
• Stellar Feedback — 18× in this paper · explained in 2 episodes
• Bulk Viscosity — 13× in this paper · explained in 2 episodes
• Momentum transfer — 9× in this paper · explained in 2 episodes
• Robustness — 7× in this paper · explained in 5 episodes
• Velocity Dispersion — 7× in this paper · explained in 2 episodes
• Ambipolar Diffusion — 6× in this paper · explained in 1 episode
• Consistency — 6× in this paper · explained in 3 episodes
• Abundance — 5× in this paper · explained in 1 episode
• Anisotropy — 4× in this paper · explained in 3 episodes
• Streaming Instability — 4× in this paper · explained in 2 episodes
• Accretion Shock — 3× in this paper · explained in 1 episode
• Angular Momentum Transport — 3× in this paper · explained in 3 episodes
• Center of Mass (CoM) — 3× in this paper · explained in 2 episodes
• Fidelity — 3× in this paper · explained in 2 episodes
• Decoupling — 2× in this paper · explained in 2 episodes
• Diffusion Model — 2× in this paper · explained in 8 episodes
• Diffusion Models — 2× in this paper · explained in 6 episodes
• Fast Fourier Transform — 2× in this paper
• Frequency Dependence — 2× in this paper · explained in 2 episodes
• Metallicity — 2× in this paper · explained in 3 episodes
• N-body simulations — 2× in this paper · explained in 2 episodes
• AGN — 1× in this paper · explained in 1 episode
• Abstraction — 1× in this paper · explained in 1 episode
• Accretion Flows — 1× in this paper · explained in 1 episode
• Adam — 1× in this paper · explained in 2 episodes
• Adaptation — 1× in this paper · explained in 1 episode
• Adaptivity — 1× in this paper · explained in 1 episode
• Alignment — 1× in this paper · explained in 1 episode
• Anisotropic Transport — 1× in this paper · explained in 1 episode
• Artificial Intelligence (AI) — 1× in this paper · explained in 2 episodes
• Benchmark — 1× in this paper · explained in 2 episodes
• Boltzmann Equation — 1× in this paper · explained in 2 episodes
• Clustering — 1× in this paper · explained in 2 episodes
• Conservation Laws — 1× in this paper · explained in 3 episodes
• Cooperation — 1× in this paper · explained in 2 episodes
• Equation of State (EoS) — 1× in this paper · explained in 4 episodes
• Initial Mass Function (IMF) — 1× in this paper · explained in 2 episodes
• Loss Function — 1× in this paper · explained in 2 episodes
• Matter Power Spectrum — 1× in this paper · explained in 2 episodes
• Over-smoothing — 1× in this paper · explained in 4 episodes
• Primordial Magnetic Fields — 1× in this paper · explained in 2 episodes
• Scaling Improvement — 1× in this paper · explained in 2 episodes
• Scaling Laws — 1× in this paper · explained in 4 episodes
• Star Formation Efficiency (SFE) — 1× in this paper · explained in 2 episodes
• Star Formation Rate (SFR) — 1× in this paper · explained in 5 episodes
• Trace — 1× in this paper · explained in 2 episodes
• Verification — 1× in this paper · explained in 2 episodes
• Zero Age Main Sequence — 1× in this paper

Sources

• Adaptive Ray Tracing for Radiative Transfer around Point Sources
• Efficient highly-subsonic turbulent dynamo and growth of primordial magnetic fields
• AHKASH: a new Hybrid particle-in-cell code for simulations of astrophysical collisionless plasma
• Critical magnetic Reynolds number of the turbulent dynamo in collisionless plasmas
• Fundamental differences between SPH and grid methods
• Birth of magnetized low-mass protostars and circumstellar disks
• Skillful joint probabilistic weather forecasting from marginals
• Formation and evolution of interstellar filaments; Hints from velocity dispersion measurements
• Molecular filament formation and filament-cloud interaction: Hints from Nobeyama 45m telescope observations
• A radiative transfer scheme for cosmological reionization based on a local Eddington tensor
• Fervent: Chemistry-coupled, ionising and non-ionising radiative feedback in magnetohydrodynamical simulations
• TreePM: A code for Cosmological N-Body Simulations
• Outflows and Jets from Collapsing Magnetized Cloud Cores
• The dependence of star formation on initial conditions and molecular cloud structure
• The Importance of Radiative Feedback for the Stellar Initial Mass Function
• Stellar, brown dwarf and multiple star properties from a radiation hydrodynamical simulation of star cluster formation
• On the diversity and statistical properties of protostellar discs
• Modelling Accretion in Protobinary Systems
• The Formation of a Star Cluster: Predicting the Properties of Stars and Brown Dwarfs
• Growth or Decay -- I: universality of the turbulent dynamo saturation

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