Hydrodynamical Code for Numerical Simulation of the Gas Components of Colliding Galaxies

Вшивков, В. А.; Lazareva, G. G.; Снытников, А. В.; Kulikov, Igor; Тутуков, А. В.

doi:10.1088/0067-0049/194/2/47

Cited by 34 publications

(14 citation statements)

References 29 publications

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“…Poisson equation solver is based on 27-point stencil and uses FFT procedure. This Poisson solver worked well during the solution of some astrophysical problems [49,51].…”

Section: Methodsmentioning

confidence: 99%

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AstroPhi: A code for complex simulation of the dynamics of astrophysical objects using hybrid supercomputers

Kulikov

Chernykh

Снытников

et al. 2015

Computer Physics Communications

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“…Poisson equation solver is based on 27-point stencil and uses FFT procedure. This Poisson solver worked well during the solution of some astrophysical problems [49,51].…”

Section: Methodsmentioning

confidence: 99%

“…Our research group has been developing the Lagrangian-Eulerian approach on the basis of the fluids in cells (FlIC) and Godunov methods for several years [3,22,[48][49][50][51]. The AstroPhi code proposed here is based on an equation solver for gas dynamics comprising two stages.…”

Section: Introductionmentioning

confidence: 99%

AstroPhi: A code for complex simulation of the dynamics of astrophysical objects using hybrid supercomputers

Kulikov

Chernykh

Снытников

et al. 2015

Computer Physics Communications

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“…This invariance appears because of the mesh. But this problem can be solved by means of the various approaches to the design of numerical schemes [9]. One of the common weak points of both Lagragian and Eulerian approaches is the lack of scalability.…”

Section: Co-design Of Parallel Numerical Methods For Astrophysicsmentioning

confidence: 99%

“…These methods combine the advantages of both Lagrangian and Eulerian approaches. For a number of years the authors have been developing the Lagrangian-Eulerian approach on the basis of the combination of the Fluid-In-Cells method and Godunov method [9,11,34,35]. The system of gas dynamics equations is solved in two stages.…”

Section: Co-design Of Parallel Numerical Methods For Astrophysicsmentioning

confidence: 99%

Co-design of Parallel Numerical Methods for Plasma Physics and Astrophysics

Glinskiy

Kulikov

Снытников

et al. 2014

JSFI

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Physically meaningful simulations in plasma physics and astrophysics need powerful hybrid supercomputers equipped with computation accelerators. The development of parallel numerical codes for such supercomputers is a complex scientific problem. In order to solve it the concept of codesign is employed. The co-design is defined as considering the architecture of the supercomputer at all stages of the development of the code. The use of co-design is shown by the example of two physical problems: the interaction of an electron beam with plasma and the collision of galaxies. The efficiency is 92 % with 500 Tesla GPUs at the Lomonosov supercomputer. The test computation involved 160 million of model particles.

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“…Switching to the total energy helps to eliminate this problem (e.g., Clarke 2010). However, in numerical codes that make use of a staggered grid as our own, with vector and scalar variables defined at different positions on the grid, solving for the total energy equation is not a good option as it inevitably requires interpolating between the internal and kinetic energies to obtain the total energy (Clarke 2010) or applying corrections after each time step to conserve the total energy (Vshivkov et al 2011). In either case, this practice, according to our experience, often comes at a cost of degraded performance on other test problems and is not recommended.…”

Section: A2 Sedov Point Explosionmentioning

confidence: 99%

Stellar hydrodynamical modeling of dwarf galaxies: simulation methodology, tests, and first results

Vorobyov

Recchi

Hensler

2015

A&A

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Context. In spite of enormous progress and brilliant achievements in cosmological simulations, they still lack numerical resolution or physical processes to simulate dwarf galaxies in sufficient detail. Accurate numerical simulations of individual dwarf galaxies are thus still in demand. Aims. We aim to improve available numerical techniques to simulate individual dwarf galaxies. In particular, we aim to (i) study in detail the coupling between stars and gas in a galaxy, exploiting the so-called stellar hydrodynamical approach; and (ii) study for the first time the chemodynamical evolution of individual galaxies starting from self-consistently calculated initial gas distributions.Methods. We present a novel chemodynamical code for studying the evolution of individual dwarf galaxies. In this code, the dynamics of gas is computed using the usual hydrodynamics equations, while the dynamics of stars is described by the stellar hydrodynamics approach, which solves for the first three moments of the collisionless Boltzmann equation. The feedback from stellar winds and dying stars is followed in detail. In particular, a novel and detailed approach has been developed to trace the aging of various stellar populations, which facilitates an accurate calculation of the stellar feedback depending on the stellar age. The code has been accurately benchmarked, allowing us to provide a recipe for improving the code performance on the Sedov test problem. Results. We build initial equilibrium models of dwarf galaxies that take gas self-gravity into account and present different levels of rotational support. Models with high rotational support (and hence high degrees of flattening) develop prominent bipolar outflows; a newly-born stellar population in these models is preferentially concentrated to the galactic midplane. Models with little rotational support blow away a large fraction of the gas and the resulting stellar distribution is extended and diffuse. Models that start from non-self-gravitating initial equilibrium configurations, evolve at a much slower pace owing to lower initial gas density and hence lower star formation rates. The stellar dynamics turns out to be a crucial aspect of galaxy evolution. If we artificially suppress stellar dynamics, supernova explosions occur in a medium that is heated and diluted by previous activity of stellar winds, thus artificially enhancing stellar feedback. Conclusions. The stellar hydrodynamics approach presents a promising tool for numerically studying the coupled evolution of gas and stars in dwarf galaxies.

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Hydrodynamical Code for Numerical Simulation of the Gas Components of Colliding Galaxies

Cited by 34 publications

References 29 publications

AstroPhi: A code for complex simulation of the dynamics of astrophysical objects using hybrid supercomputers

AstroPhi: A code for complex simulation of the dynamics of astrophysical objects using hybrid supercomputers

Co-design of Parallel Numerical Methods for Plasma Physics and Astrophysics

Stellar hydrodynamical modeling of dwarf galaxies: simulation methodology, tests, and first results

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