8,208 research outputs found
Numerical solutions of the three-dimensional magnetohydrodynamic alpha-model
We present direct numerical simulations and alpha-model simulations of four
familiar three-dimensional magnetohydrodynamic (MHD) turbulence effects:
selective decay, dynamic alignment, inverse cascade of magnetic helicity, and
the helical dynamo effect. The MHD alpha-model is shown to capture the
long-wavelength spectra in all these problems, allowing for a significant
reduction of computer time and memory at the same kinetic and magnetic Reynolds
numbers. In the helical dynamo, not only does the alpha-model correctly
reproduce the growth rate of magnetic energy during the kinematic regime, but
it also captures the nonlinear saturation level and the late generation of a
large scale magnetic field by the helical turbulence.Comment: 12 pages, 19 figure
Adaptive Mesh Fluid Simulations on GPU
We describe an implementation of compressible inviscid fluid solvers with
block-structured adaptive mesh refinement on Graphics Processing Units using
NVIDIA's CUDA. We show that a class of high resolution shock capturing schemes
can be mapped naturally on this architecture. Using the method of lines
approach with the second order total variation diminishing Runge-Kutta time
integration scheme, piecewise linear reconstruction, and a Harten-Lax-van Leer
Riemann solver, we achieve an overall speedup of approximately 10 times faster
execution on one graphics card as compared to a single core on the host
computer. We attain this speedup in uniform grid runs as well as in problems
with deep AMR hierarchies. Our framework can readily be applied to more general
systems of conservation laws and extended to higher order shock capturing
schemes. This is shown directly by an implementation of a magneto-hydrodynamic
solver and comparing its performance to the pure hydrodynamic case. Finally, we
also combined our CUDA parallel scheme with MPI to make the code run on GPU
clusters. Close to ideal speedup is observed on up to four GPUs.Comment: Submitted to New Astronom
Three Dimensional Pseudo-Spectral Compressible Magnetohydrodynamic GPU Code for Astrophysical Plasma Simulation
This paper presents the benchmarking and scaling studies of a GPU accelerated
three dimensional compressible magnetohydrodynamic code. The code is developed
keeping an eye to explain the large and intermediate scale magnetic field
generation is cosmos as well as in nuclear fusion reactors in the light of the
theory given by Eugene Newman Parker. The spatial derivatives of the code are
pseudo-spectral method based and the time solvers are explicit. GPU
acceleration is achieved with minimal code changes through OpenACC
parallelization and use of NVIDIA CUDA Fast Fourier Transform library (cuFFT).
NVIDIAs unified memory is leveraged to enable over-subscription of the GPU
device memory for seamless out-of-core processing of large grids. Our
experimental results indicate that the GPU accelerated code is able to achieve
upto two orders of magnitude speedup over a corresponding OpenMP parallel, FFTW
library based code, on a NVIDIA Tesla P100 GPU. For large grids that require
out-of-core processing on the GPU, we see a 7x speedup over the OpenMP, FFTW
based code, on the Tesla P100 GPU. We also present performance analysis of the
GPU accelerated code on different GPU architectures - Kepler, Pascal and Volta
Spectral features of solar wind turbulent plasma
Spectral properties of a fully compressible solar wind Hall
Magnetohydrodynamic plasma are investigated by means of time dependent three
dimensional Hall MHD simulations. Our simulations, in agreement with spacecraft
data, identify a spectral break in turbulence spectra at characteristic
length-scales associated with electromagnetic fluctuations that are smaller
than the ion gyroradius. In this regime, our 3D simulations show that turbulent
spectral cascades in the presence of a mean magnetic field follow an
omnidirectional anisotropic inertial range spectrum close to . The
onset of the spectral break in our simulations can be ascribed to the presence
of nonlinear Hall interactions that modify the spectral cascades. Our
simulations further show that the underlying charachteristic turbulent
fluctuations are spectrally anisotropic, the extent of which depends critically
on the local wavenumber. The fluctuations associated with length scales smaller
than the ion gyroradius are highly compressible and tend to exhibit a near
equipartition in the velocity and magnetic fields. Finally, we find that the
orientation of velocity and magnetic field fluctuations critically determine
the character of nonlinear interactions that predominantly govern a Hall MHD
plasma, like the solar wind.Comment: This paper is accepted for publication in Monthly Notices of the
Royal Astronomical Society Main Journa
Non regression testing for the JOREK code
Non Regression Testing (NRT) aims to check if software modifications result
in undesired behaviour. Suppose the behaviour of the application previously
known, this kind of test makes it possible to identify an eventual regression,
a bug. Improving and tuning a parallel code can be a time-consuming and
difficult task, especially whenever people from different scientific fields
interact closely. The JOREK code aims at investing Magnetohydrodynamic (MHD)
instabilities in a Tokamak plasma. This paper describes the NRT procedure that
has been tuned for this simulation code. Automation of the NRT is one keypoint
to keeping the code healthy in a source code repository.Comment: No. RR-8134 (2012
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