scholarly journals The formation of entropy cores in non-radiative galaxy cluster simulations: smoothed particle hydrodynamics versus adaptive mesh refinement

2014 ◽  
Vol 440 (4) ◽  
pp. 3243-3256 ◽  
Author(s):  
C. Power ◽  
J. I. Read ◽  
A. Hobbs
Keyword(s):  
Smoothed Particle Hydrodynamics ◽  
Adaptive Mesh Refinement ◽  
Mesh Refinement ◽  
Galaxy Cluster ◽  
Adaptive Mesh ◽  
Particle Hydrodynamics ◽  
Smoothed Particle

scholarly journals Numerical Hydrodynamics: SPH versus AMR

2001 ◽  
Vol 200 ◽  
pp. 563-566
Author(s):  
Tomek Plewa
Keyword(s):  
Smoothed Particle Hydrodynamics ◽  
Adaptive Mesh Refinement ◽  
Mesh Refinement ◽  
Adaptive Mesh ◽  
Computational Hydrodynamics ◽  
Advantages And Disadvantages ◽  
Numerical Hydrodynamics ◽  
Particle Hydrodynamics ◽  
Smoothed Particle

The advantages and disadvantages of two approaches to astrophysical hydrodynamics, Smoothed Particle Hydrodynamics (SPH) and Adaptive Mesh Refinement (AMR), are briefly discussed together with some current problems of computational hydrodynamics.

scholarly journals Hydrodynamical Adaptive Mesh Refinement Simulations of Disk Galaxies

2008 ◽  
Vol 4 (S254) ◽  
pp. 445-452
Author(s):  
Brad K. Gibson ◽  
Stéphanie Courty ◽  
Patricia Sánchez-Blázquez ◽  
Romain Teyssier ◽  
Elisa L. House ◽  
...  
Keyword(s):  
Galaxy Formation ◽  
Adaptive Mesh Refinement ◽  
Mesh Refinement ◽  
Adaptive Mesh ◽  
Disk Galaxies ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Temporal And Spatial ◽  
Compare And Contrast

AbstractTo date, fully cosmological hydrodynamic disk simulations to redshift zero have only been undertaken with particle-based codes, such as GADGET, Gasoline, or GCD+. In light of the (supposed) limitations of traditional implementations of smoothed particle hydrodynamics (SPH), or at the very least, their respective idiosyncrasies, it is important to explore complementary approaches to the SPH paradigm to galaxy formation. We present the first high-resolution cosmological disk simulations to redshift zero using an adaptive mesh refinement (AMR)-based hydrodynamical code, in this case, RAMSES. We analyse the temporal and spatial evolution of the simulated stellar disks' vertical heating, velocity ellipsoids, stellar populations, vertical and radial abundance gradients (gas and stars), assembly/infall histories, warps/lopsideness, disk edges/truncations (gas and stars), ISM physics implementations, and compare and contrast these properties with our sample of cosmological SPH disks, generated with GCD+. These preliminary results are the first in our long-term Galactic Archaeology Simulation program.

scholarly journals Convergence of SPH and AMR simulations

2010 ◽  
Vol 6 (S270) ◽  
pp. 429-432
Author(s):  
David A. Hubber ◽  
Sam A. E. G. Falle ◽  
Simon P. Goodwin
Keyword(s):  
Smoothed Particle Hydrodynamics ◽  
Thin Shell ◽  
Adaptive Mesh Refinement ◽  
Adaptive Mesh ◽  
Helmholtz Instability ◽  
Non Linear ◽  
Particle Hydrodynamics ◽  
First Results ◽  
Order Of Magnitude ◽  
Smoothed Particle

AbstractWe present the first results of a large suite of convergence tests between Adaptive Mesh Refinement (AMR) Finite Difference Hydrodynamics and Smoothed Particle Hydrodynamics (SPH) simulations of the non-linear thin shell instability and the Kelvin-Helmholtz instability. We find that the two methods converge in the limit of high resolution and accuracy. AMR and SPH simulations of the non-linear thin shell instability converge with each other with standard algorithms and parameters. The Kelvin-Helmholtz instability in SPH requires both an artificial conductivity term and a kernel with larger compact support and more neighbours (e.g. the quintic kernel) in order converge with AMR. For purely hydrodynamical problems, SPH simulations take an order of magnitude longer than the grid code when converged.

scholarly journals Implementing and comparing sink particles in AMR and SPH

2010 ◽  
Vol 6 (S270) ◽  
pp. 425-428 ◽  
Author(s):  
Christoph Federrath ◽  
Robi Banerjee ◽  
Daniel Seifried ◽  
Paul C. Clark ◽  
Ralf S. Klessen
Keyword(s):  
Star Formation ◽  
Adaptive Mesh Refinement ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Particle Creation ◽  
Adaptive Mesh ◽  
Particle Properties ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Density Threshold

AbstractWe implemented sink particles in the Adaptive Mesh Refinement (AMR) code FLASH to model the gravitational collapse and accretion in turbulent molecular clouds and cores. Sink particles are frequently used to measure properties of star formation in numerical simulations, such as the star formation rate and efficiency, and the mass distribution of stars. We show that only using a density threshold for sink particle creation is insufficient in case of supersonic flows, because the density can exceed the threshold in strong shocks that do not necessarily lead to local collapse. Additional physical collapse indicators have to be considered. We apply our AMR sink particle module to the formation of a star cluster, and compare it to a Smoothed Particle Hydrodynamics (SPH) code with sink particles. Our comparison shows encouraging agreement of gas and sink particle properties between the AMR and SPH code.

scholarly journals GALAXY CLUSTER RADIO RELICS IN ADAPTIVE MESH REFINEMENT COSMOLOGICAL SIMULATIONS: RELIC PROPERTIES AND SCALING RELATIONSHIPS

2011 ◽  
Vol 735 (2) ◽  
pp. 96 ◽  
Author(s):  
Samuel W. Skillman ◽  
Eric J. Hallman ◽  
Brian W. O'Shea ◽  
Jack O. Burns ◽  
Britton D. Smith ◽  
...  
Keyword(s):  
Adaptive Mesh Refinement ◽  
Mesh Refinement ◽  
Galaxy Cluster ◽  
Adaptive Mesh ◽  
Cosmological Simulations ◽  
Scaling Relationships

Three-dimensional modelling of Uttarakhand slides using smoothed particle hydrodynamics (SPH)

2021 ◽  
Author(s):  
Shuai Li ◽  
Hui Tang ◽  
Chong Peng ◽  
Hui-Cong An
Keyword(s):  
Smoothed Particle Hydrodynamics ◽  
Frictional Heating ◽  
Three Dimensional ◽  
Time History ◽  
Adaptive Mesh ◽  
High Water ◽  
High Water Content ◽  
Mesh Free ◽  
Particle Hydrodynamics ◽  
Smoothed Particle

<p>On 7 February 2021, a massive flood occurred in the river Dhauliganga that damaged two hydroelectric stations, five bridges and trapped 100 to 150 casualties who are feared dead. Some evidence has been indicated that caused by a landslide, an avalanche, or a portion of the Nanda Devi glacier that broke off early in Uttarakhand's Joshimath area Chamoli district. The magnitude of the flood caused by the collapse was so large that it far exceeds the collapse itself. Two potential explanations were proposed to explain: the frictional heating of the avalanche may result in high temperatures in the sliding face, which is sufficient for ice and frozen sediments melting to occur in the path. The high-water content generated debris flows that enhanced the mobility of flowing. Another explanation is that it could be related to a glacial lake outburst flood or a temporary lake that eventually broke through its debris dam and poured down the valley. In any case, the collapse materials hold very high moisture content and fast mobility. In this study, a three-dimensional Smoothed Particle Hydrodynamics (SPH) method is adopted to model the flow-like Uttarakhand slides and to explore the physical processes during this event. The SPH is an adaptive, mesh-free, Lagrangian method that simulates free surfaces, moving interfaces, and large flow deformations. A non-Newtonian debris flow model, the Bingham rheological relationship, was incorporated into the SPH framework to describe source materials' characteristics. Besides, the whole flow processes of the flow-like Uttarakhand slides across the 3D terrain are represented. The time history of the velocity, acceleration, and forces were obtained from modelling to analyze the landslide dynamics.</p>

scholarly journals Faint rapid red transients from neutron star–CO white dwarf mergers

2020 ◽  
Vol 493 (3) ◽  
pp. 3956-3965 ◽  
Author(s):  
Yossef Zenati ◽  
Alexey Bobrick ◽  
Hagai B Perets
Keyword(s):  
Adaptive Mesh Refinement ◽  
Radiation Transfer ◽  
Adaptive Mesh ◽  
Light Curves ◽  
Post Process ◽  
Type Ia ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Transient Events ◽  
Ia Supernovae

ABSTRACT Mergers of neutron stars (NS) and white dwarfs (WD) may give rise to observable explosive transient events. We use 3D hydrodynamical (smoothed particle hydrodynamics – SPH) simulations and 2D hydrodynamical–thermonuclear simulations (using the flash adaptive mesh refinement code) to model the disruption of CO-WDs by NSs, which produce faint transient events. We post-process the simulations using a large nuclear network and make use of the SuperNu radiation transfer code to predict the observational signatures and detailed properties of these transients. We calculate the light curves and spectra for five models of NS–CO-WD mergers. The small yields of 56Ni (few $\times 10^{-3}\, {\rm M_{\odot }}$) result in faint, rapidly evolving reddened transients (RRTs) with B(R) peak magnitudes of at most ∼−12 (−13) to ∼−13 (−15), much shorter and fainter than both regular and faint/peculiar Type Ia supernovae. These transients are likely to be accompanied by several months long, 1–2 mag dimmer red/infrared afterglows. We show that the spectra of RRTs share some similarities with rapidly evolving transients such as SN 2010X, although RRTs are significantly fainter, especially in the I/R bands, and show far stronger Si lines. We estimate that the upcoming Large Synoptic Survey Telescope could detect RRTs at a rate of up to ∼10–70 yr−1 through observations in the R/I bands. The qualitative agreement between the SPH and flash approaches supports the earlier hydrodynamical studies of these systems.

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