Enzo: An Adaptive Mesh Refinement Code for Astrophysics

Bryan, Greg L.; Norman, Michael L.; O’Shea, Brian W.; Abel, Tom; Wise, John H.; Turk, Matthew J.; Reynolds, Daniel R.; Collins, David C.; Wang, Peng; Skillman, Samuel W.; Smith, Britton D.; Harkness, Robert; Bordner, James; Kim, Ji-hoon; Kuhlen, M.; Xu, Hao; Goldbaum, Nathan J.; Hummels, Cameron; Kritsuk, Alexei G.; Tasker, Elizabeth J.; Skory, Stephen; Simpson, Christine M.; Hahn, Oliver; Oishi, Jeffrey S.; So, Geoffrey C.; Zhao, Fei; Cen, Renyue; Li, Yuan

doi:10.1088/0067-0049/211/2/19

Cited by 756 publications

(624 citation statements)

References 186 publications

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“…We used a modified version of the grid-based hydrodynamics code enzo (O'Shea et al 2004;Passy et al 2012a;Bryan et al 2014) to run the hydrodynamics simulations. The calculations were performed on a 256 3 grid in the adiabatic approximation with outflow boundary conditions.…”

Section: Methodsmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

126

100

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We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zeroage main sequence mass of 3.5 M ⊙ . Dynamic in-spiral timescales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars' envelopes are somewhat puffed up. Based on relatively long timescales and even considering the fact that further inspiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star-planet interaction may be unable to lead to large scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.

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Section: Methodsmentioning

confidence: 99%

Hydrodynamic simulations of the interaction between giant stars and planets

Staff

Marco

Wood

et al. 2016

Mon. Not. R. Astron. Soc.

126

100

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“…We carried out, using the publicly available ENZO code (Bryan et al 2014), multiple cosmological simulations designed to follow closely the formation of clusters selected to have a broad range of evolutionary histories.…”

Section: Simulationsmentioning

confidence: 99%

Turbulence and vorticity in Galaxy clusters generated by structure formation

Vazza

Jones

Brüggen

et al. 2016

Mon. Not. R. Astron. Soc.

113

149

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Turbulence is a key ingredient for the evolution of the intracluster medium, whose properties can be predicted with high resolution numerical simulations. We present initial results on the generation of solenoidal and compressive turbulence in the intracluster medium during the formation of a small-size cluster using highly resolved, non-radiative cosmological simulations, with a refined monitoring in time. In this first of a series of papers, we closely look at one simulated cluster whose formation was distinguished by a merger around z ∼ 0.3. We separate laminar gas motions, turbulence and shocks with dedicated filtering strategies and distinguish the solenoidal and compressive components of the gas flows using Hodge-Helmholtz decomposition. Solenoidal turbulence dominates the dissipation of turbulent motions (∼ 95%) in the central cluster volume at all epochs. The dissipation via compressive modes is found to be more important (∼ 30% of the total) only at large radii ( 0.5 r vir ) and close to merger events. We show that enstrophy (vorticity squared) is good proxy of solenoidal turbulence. All terms ruling the evolution of enstrophy (i.e. baroclinic, compressive, stretching and advective terms) are found to be significant, but in amounts that vary with time and location. Two important trends for the growth of enstrophy in our simulation are identified: first, enstrophy is continuously accreted into the cluster from the outside, and most of that accreted enstrophy is generated near the outer accretion shocks by baroclinic and compressive processes. Second, in the cluster interior vortex stretching is dominant, although the other terms also contribute substantially.

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“…We use the numerical code Enzo 6 , a magnetohydrodynamics (MHD) adaptive mesh refinement (AMR) code (Bryan et al 2014). This code solves the MHD equations using the MUSCL second-order Runge-Kutta temporal update of the conserved variables with the Harten-Lax-van Leer with Discontinuities (HLLD) method and a piecewise linear reconstruction method.…”

Section: Numerical Codementioning

confidence: 99%

“…The resulting heating and cooling rates are incorporated into Enzo via the Grackle external chemistry and cooling library 7 (Bryan et al 2014;Kim et al 2014). The information is read in via the purely tabulated method and modifies the gas internal energy,…”

Section: Thermal Processesmentioning

confidence: 99%

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GMC Collisions as Triggers of Star Formation. II. 3D Turbulent, Magnetized Simulations

Tan

Nakamura

et al. 2017

ApJ

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We investigate giant molecular cloud collisions and their ability to induce gravitational instability and thus star formation. This mechanism may be a major driver of star formation activity in galactic disks. We carry out a series of 3D, magnetohydrodynamics (MHD), adaptive mesh refinement simulations to study how cloud collisions trigger formation of dense filaments and clumps. Heating and cooling functions are implemented based on photodissociation region models that span the atomic-to-molecular transition and can return detailed diagnostic information. The clouds are initialized with supersonic turbulence and a range of magnetic field strengths and orientations. Collisions at various velocities and impact parameters are investigated. Comparing and contrasting colliding and non-colliding cases, we characterize morphologies of dense gas, magnetic field structure, cloud kinematic signatures, and cloud dynamics. We present key observational diagnostics of cloud collisions, especially: relative orientations between magnetic fields and density structures, like filaments; 13 CO( J=2-1), 13 CO( J=3-2), and 12 CO( J=8-7) integrated intensity maps and spectra; and cloud virial parameters. We compare these results to observed Galactic clouds.

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Enzo: An Adaptive Mesh Refinement Code for Astrophysics

Cited by 756 publications

References 186 publications

Hydrodynamic simulations of the interaction between giant stars and planets

Hydrodynamic simulations of the interaction between giant stars and planets

Turbulence and vorticity in Galaxy clusters generated by structure formation

GMC Collisions as Triggers of Star Formation. II. 3D Turbulent, Magnetized Simulations

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