Smoothed-Particle Hydrodynamics Models: Implementation Features on GPUs

Khrapov, S. S.; Хоперсков, А. В.

doi:10.1007/978-3-319-71255-0_21

Cited by 15 publications

(22 citation statements)

References 13 publications

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“…The generation of the model initial equlibrium follows an iterative method of the Jeans equation solution (Khoperskov et al 2012). The simulation was performed with a direct GPU N-body/SPH code which provides a very high accuracy of the numerical integration (Khrapov & Khoperskov 2017). We focus our analysis on a single snapshot of the evolution at 1.3 Gyr when an extended multi-arm tightly-wound spiral structure is formed in the model.…”

Section: Appendix A: Galaxy Models: Understanding the Milky Way Guidimentioning

confidence: 99%

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

Khoperskov

Gerhard

Matteo

et al. 2020

A&A

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In this paper we introduce a new method for analysing Milky Way phase-space which allows us to reveal the imprint left by the Milky Way bar and spiral arms in the stars with full phase-space data in Gaia Data Release 2. The unprecedented quality and extended spatial coverage of these data enable us to discover six prominent stellar density structures in the disc to a distance of 5 kpc from the Sun. Four of these structures correspond to the spiral arms detected previously in the gas and young stars (Scutum-Centaurus, Sagittarius, Local and Perseus), while the remaining two are associated with two main resonances of the Milky Way bar. For the first time we provide evidence of the imprint left by spiral arms and resonances in the stellar densities not relying on a specific tracer, through a mean of enhancing the signatures left by these asymmetries. Our method offers new avenues for studying how the stellar populations in our Galaxy are shaped. Article number, page 2 of 10 S. Khoperskov et al.: Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2 Model I Milky Way -Gaia DR2 Model II

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Section: Appendix A: Galaxy Models: Understanding the Milky Way Guidimentioning

confidence: 99%

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

Khoperskov

Gerhard

Matteo

et al. 2020

A&A

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“…The maximum speedup of parallel computing for OpenMP strongly depends on the CPU Type and varies from 1.8 to 11 for different CPUs. Mass transfer of regional climate models to GPUs is a priority task in accordance with the general trend of development of computational fluid dynamics [3].…”

Section: Discussionmentioning

confidence: 99%

Regional Climate Model for the Lower Volga: Parallelization Efficiency Estimation

2018

JSFI

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We have deployed the regional climate model (RCM) RegCM 4.5 for the Lower Volga and adjacent territories with a horizontal spatial resolution of 20 km. The problems of choosing the computational domain in the RCM RegCM version 4.5 are considered. We demonstrate the influence of this factor on the forecast of rainfall distribution in the numerical simulations. The study of rainfall and snowfall is a more demanding test in comparison with temperature or pressure distributions. We investigate dependencies of calculation time, parallel speedup and parallelization efficiency on the number of processes for different multi-core CPUs. Our analysis of the efficiency of parallel implementation of RegCM for various multi-core and multi-processor systems show a strong dependence of the simulation speed on the CPU type. The best effect is achieved when the number of CPU threads and the number of parallel processes are equal. The parallel code speedup is in the range of 1.8-11 for different CPUs.

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“…We use a parallel algorithm to solving the N-body + SPH problems based on the hybrid technology OpenMP-CUDA with the number of particles N = 10 5 − 10 7 . A detailed description of the numerical algorithms SPH and N-body is given in papers [28,29]. In the papers [30,31] it was also noted that the result of the parallel software implementation and its efficiency depends on the details of the code and on the sequence of the numerical operations.…”

Section: Numerical Code and Parametersmentioning

confidence: 99%

Numerical Modelling of the Dynamics of the Galactic Halos in the Colliding Galaxies

Khrapov¹,

Хоперсков²,

Корчагин³

2019

Bulletin SUSU MMP

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Based on parallel three-dimensional simulation of N-body and gas self-consistent dynamics, we study the behavior of hot coronal gas in the colliding galaxies with "live" dark matter halos. We model a few scenarios of the galactic collisions including "bull-eye" and non-central ones, and use different values of the initial velocities of the colliding galaxies. Taking into account the self-gravity, we demonstrate that the collision of gaseous and stellar components does not lead to the formation of a gaseous "protogalaxy" observed in some numerical simulations. Also, we show that about sixty percent of hot halo gas is expelled into intergalactic space during the collision. Numerical simulations show that a considerable amount of gas (up to 70% for a bull-eye collisions) exchanges between two colliding galaxies.

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Smoothed-Particle Hydrodynamics Models: Implementation Features on GPUs

Cited by 15 publications

References 13 publications

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2

Regional Climate Model for the Lower Volga: Parallelization Efficiency Estimation

Numerical Modelling of the Dynamics of the Galactic Halos in the Colliding Galaxies

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