Elizabeth J. Tasker

TL;DR: Enzo as discussed by the authors uses block-structured adaptive mesh refinement to provide high spatial and temporal resolution for modeling astrophysical fluid flows, which can be run in one, two, and three dimensions, and supports a wide variety of physics, including hydrodynamics, ideal and non-ideal magnetohydrodynamic, N-body dynamics, primordial gas chemistry, optically thin radiative cooling of primordial and metal-enriched plasmas, and models for star formation and feedback in a cosmological context.

TL;DR: Enzo as mentioned in this paper uses block-structured adaptive mesh refinement to provide high spatial and temporal resolution for modeling astrophysical fluid flows, which can be run in 1, 2, and 3 dimensions, and supports a wide variety of physics, including hydrodynamics, ideal and non-ideal magnetohydrodynamic, N-body dynamics, primordial gas chemistry, optically-thin radiative cooling of primordial and metal-enriched plasmas, and models for star formation and feedback.

TL;DR: In this paper, a comparison of grid and smoothed particle hydrodynamics (SPH) techniques for interacting multiphase fluids is carried out, and it is shown that SPH introduces spurious pressure forces on particles in regions where there are steep density gradients.

TL;DR: Enzo as discussed by the authors uses block-structured adaptive mesh refinement to provide high spatial and temporal resolution for modeling astrophysical fluid flows, which can be run in one, two, and three dimensions, and supports a wide variety of physics, including hydrodynamics, ideal and non-ideal magnetohydrodynamic, N-body dynamics, primordial gas chemistry, optically thin radiative cooling of primordial and metal-enriched plasmas, and models for star formation and feedback in a cosmological context.

TL;DR: In this paper, the authors performed sub-parsec scale simulations of two idealized molecular clouds with different masses undergoing a collision and investigated the effect of turbulence and collision speed on the resulting core population and compared the cumulative mass distribution to cores in observed GMCs.