Stellar Hydrodynamics Simulations

Welcome Image — Vorticity (curl derivative of velocity) in a 25M_⊙ 3D stellar hydrodynamics simulation. The central bright red region is the turbulent convective core. The blue regions are the stable radiative zone that is filled with internal gravity waves. This run (M115) along with several others are reported in: Herwig et al. 2023. 3D hydrodynamic simulations of massive main-sequence stars - I. Dynamics and mixing of convection and internal gravity waves. *MNRAS.* 525:1601.

More information on stellar hydrodynamics simulations can be found on our virtual research platform PPMstar.org hosted on the Digital Alliance cloud computing Arbutus machine operated by the University of Victoria Research Computing Services.

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