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Title: Smoothed Particle Hydrodynamic Simulator

Abstract

This code is a highly modular framework for developing smoothed particle hydrodynamic (SPH) simulations running on parallel platforms. The compartmentalization of the code allows for rapid development of new SPH applications and modifications of existing algorithms. The compartmentalization also allows changes in one part of the code used by many applications to instantly be made available to all applications.

Publication Date:
Research Org.:
Pacific Northwest National Lab. (PNNL), Richland, WA (United States)
Sponsoring Org.:
USDOE
OSTI Identifier:
1327945
Report Number(s):
Smoothed Particle Hydrodynamic Simulator; 004959WKSTN00
Battelle IPID 30924-E
DOE Contract Number:
AC05-76RL01830
Resource Type:
Software
Software Revision:
00
Software Package Number:
004959
Software CPU:
WKSTN
Open Source:
Yes
OSI-approved OSS license
Source Code Available:
Yes
Related Software:
Global Arrays
Country of Publication:
United States

Citation Formats

. Smoothed Particle Hydrodynamic Simulator. Computer software. https://www.osti.gov//servlets/purl/1327945. Vers. 00. USDOE. 5 Oct. 2016. Web.
. (2016, October 5). Smoothed Particle Hydrodynamic Simulator (Version 00) [Computer software]. https://www.osti.gov//servlets/purl/1327945.
. Smoothed Particle Hydrodynamic Simulator. Computer software. Version 00. October 5, 2016. https://www.osti.gov//servlets/purl/1327945.
@misc{osti_1327945,
title = {Smoothed Particle Hydrodynamic Simulator, Version 00},
author = {},
abstractNote = {This code is a highly modular framework for developing smoothed particle hydrodynamic (SPH) simulations running on parallel platforms. The compartmentalization of the code allows for rapid development of new SPH applications and modifications of existing algorithms. The compartmentalization also allows changes in one part of the code used by many applications to instantly be made available to all applications.},
url = {https://www.osti.gov//servlets/purl/1327945},
doi = {},
year = 2016,
month = ,
note =
}

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  • In this work the Smoothed Particle Hydrodynamics (SPH) method is used to simulate iron ore pellets flow. A continuum material model describing the yield strength, elastic and plastic parameters for pellets as a granular material is used in the simulations. The most time consuming part in the SPH method is the contact search of neighboring nodes at each time step. In this study, a position code algorithm for the contact search is presented. The cost of contact searching for this algorithm is of the order of Nlog2N, where N is the number of nodes in the system. The SPH-model ismore » used for simulation of iron ore pellets silo flow. A two dimensional axisymmetric model of the silo is used in the simulations. The simulation results are compared with data from an experimental cylindrical silo, where pellets are discharged from a concentric outlet. Primary the flow pattern is compared.« less
  • We examine the effect of mass and force resolution on a specific star formation (SF) recipe using a set of N-body/smooth particle hydrodynamic simulations of isolated galaxies. Our simulations span halo masses from 10{sup 9} to 10{sup 13} M{sub sun}, more than 4 orders of magnitude in mass resolution, and 2 orders of magnitude in the gravitational softening length, {epsilon}, representing the force resolution. We examine the total global SF rate, the SF history, and the quantity of stellar feedback and compare the disk structure of the galaxies. Based on our analysis, we recommend using at least 10{sup 4} particlesmore » each for the dark matter (DM) and gas component and a force resolution of {epsilon} {approx} 10{sup -3} R{sub vir} when studying global SF and feedback. When the spatial distribution of stars is important, the number of gas and DM particles must be increased to at least 10{sup 5} of each. Low-mass resolution simulations with fixed softening lengths show particularly weak stellar disks due to two-body heating. While decreasing spatial resolution in low-mass resolution simulations limits two-body effects, density and potential gradients cannot be sustained. Regardless of the softening, low-mass resolution simulations contain fewer high density regions where SF may occur. Galaxies of approximately 10{sup 10} M{sub sun} display unique sensitivity to both mass and force resolution. This mass of galaxy has a shallow potential and is on the verge of forming a disk. The combination of these factors gives this galaxy the potential for strong gas outflows driven by supernova feedback and makes it particularly sensitive to any changes to the simulation parameters.« less
  • We study the relationship between the metallicity of gamma-ray burst (GRB) progenitors and the probability distribution function (PDF) of GRB host galaxies as a function of luminosity using cosmological hydrodynamic simulations of galaxy formation. We impose a maximum limit to the gas metallicity in which GRBs can occur and examine how the predicted luminosity PDF of GRB host galaxies changes in the simulation. We perform the Kolmogorov-Smirnov test and show that the result from our simulation agrees with the observed luminosity PDF of core-collapse supernovae (SNe) host galaxies when we assume that the core-collapse SNe trace star formation. When wemore » assume that GRBs occur only in a low-metallicity environment with Z {approx}< 0.1 Z{sub sun}, GRBs occur in lower luminosity galaxies, and the simulated luminosity PDF becomes quantitatively consistent with the observed one. The observational bias against the host galaxies of optically dark GRBs owing to dust extinction may be another reason for the lower luminosities of GRB host galaxies, but the observed luminosity PDF of GRB host galaxies cannot be reproduced solely by the dust bias in our simulation.« less

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