113,786 research outputs found
The Convergence of Difference Boxes
We consider an elementary mathematical puzzle known as a difference box in terms of a discrete map from R4 to R4 or, canonically, from a subset of the first quadrant of R2 into itself. We find the map\u27s unique canonical fixed point and answer the general question of how many iterations a given difference box takes to reach zero
Measuring the three-dimensional shear from simulation data, with applications to weak gravitational lensing
We have developed a new three-dimensional algorithm, based on the standard
PM method, for computing deflections due to weak gravitational lensing. We
compare the results of this method with those of the two-dimensional planar
approach, and rigorously outline the conditions under which the two approaches
are equivalent. Our new algorithm uses a Fast Fourier Transform convolution
method for speed, and has a variable softening feature to provide a realistic
interpretation of the large-scale structure in a simulation. The output values
of the code are compared with those from the Ewald summation method, which we
describe and develop in detail. With an optimal choice of the high frequency
filtering in the Fourier convolution, the maximum errors, when using only a
single particle, are about 7 per cent, with an rms error less than 2 per cent.
For ensembles of particles, used in typical -body simulations, the rms
errors are typically 0.3 per cent. We describe how the output from the
algorithm can be used to generate distributions of magnification, source
ellipticity, shear and convergence for large-scale structure.Comment: 22 pages, latex, 11 figure
The Effect of Large-Scale Power on Simulated Spectra of the Lya forest
We study the effects of box size on ENZO simulations of the intergalactic
medium (IGM) at z = 2. We follow statistics of the cold dark matter (CDM) and
the Lya absorption. We find that the larger boxes have fewer pixels with
significant absorption (flux < 0.96) and more pixels in longer stretches with
little or no absorption, and they have wider Lya lines. We trace these effect
back to the additional power in larger boxes from longer wavelength modes. The
IGM in our larger boxes is hotter, from increased pressure heating due to
faster hydrodynamical infall. When we increase the photoheating in smaller
boxes to compensate, their Lya statistics change to mimic those of a box of
twice the size. Statistics converge towards their value in the largest (76.8
Mpc) box, except for the most common value of the CDM density which continues
to rise. When we compare to errors with data, we find that our 76.8 Mpc box is
larger than we need for the mean flux, barely large enough for the column
density distribution and the power spectrum of the flux, and too small for the
line widths. This box with 75 kpc cells has approximately the same mean flux as
QSO spectra, but the Lya lines are too wide by 2.6 km/s, there are too few
lines with log H I column densities > 10^17 cm^-2, and the power of the flux is
too low by 20 - 50%, from small to large scales. Four times smaller cell size
does not resolve these differences, nor do simple changes to the ultraviolet
background that drives the H and He II ionization. It is hard to see how
simulations using popular cosmological and astrophysical parameters can match
Lyman-alpha forest data at z=2
GRChombo : Numerical Relativity with Adaptive Mesh Refinement
In this work, we introduce GRChombo: a new numerical relativity code which
incorporates full adaptive mesh refinement (AMR) using block structured
Berger-Rigoutsos grid generation. The code supports non-trivial
"many-boxes-in-many-boxes" mesh hierarchies and massive parallelism through the
Message Passing Interface (MPI). GRChombo evolves the Einstein equation using
the standard BSSN formalism, with an option to turn on CCZ4 constraint damping
if required. The AMR capability permits the study of a range of new physics
which has previously been computationally infeasible in a full 3+1 setting,
whilst also significantly simplifying the process of setting up the mesh for
these problems. We show that GRChombo can stably and accurately evolve standard
spacetimes such as binary black hole mergers and scalar collapses into black
holes, demonstrate the performance characteristics of our code, and discuss
various physics problems which stand to benefit from the AMR technique.Comment: 48 pages, 24 figure
A New Algorithm for Computing Statistics of Weak Lensing by Large-Scale Structure
We describe an efficient algorithm for calculating the statistics of weak
lensing by large-scale structure based on a tiled set of independent
particle-mesh N-body simulations which telescope in resolution along the line
of sight. This efficiency allows us to predict not only the mean properties of
lensing observables such as the power spectrum, skewness and kurtosis of the
convergence, but also their sampling errors for finite fields of view, which
are themselves crucial for assessing the cosmological significance of
observations. We find that the nongaussianity of the distribution substantially
increases the sampling errors for the skewness and kurtosis in the several to
tens of arcminutes regime, whereas those for the power spectrum are only
fractionally increased even out to wavenumbers where shot noise from the
intrinsic ellipticities of the galaxies will likely dominate the errors.Comment: 12 pages, 13 figures; minor changes reflect accepted versio
Binary black holes on a budget: Simulations using workstations
Binary black hole simulations have traditionally been computationally very
expensive: current simulations are performed in supercomputers involving dozens
if not hundreds of processors, thus systematic studies of the parameter space
of binary black hole encounters still seem prohibitive with current technology.
Here we show how the multi-layered refinement level code BAM can be used on
dual processor workstations to simulate certain binary black hole systems. BAM,
based on the moving punctures method, provides grid structures composed of
boxes of increasing resolution near the center of the grid. In the case of
binaries, the highest resolution boxes are placed around each black hole and
they track them in their orbits until the final merger when a single set of
levels surrounds the black hole remnant. This is particularly useful when
simulating spinning black holes since the gravitational fields gradients are
larger. We present simulations of binaries with equal mass black holes with
spins parallel to the binary axis and intrinsic magnitude of S/m^2= 0.75. Our
results compare favorably to those of previous simulations of this particular
system. We show that the moving punctures method produces stable simulations at
maximum spatial resolutions up to M/160 and for durations of up to the
equivalent of 20 orbital periods.Comment: 20 pages, 8 figures. Final version, to appear in a special issue of
Class. Quantum Grav. based on the New Frontiers in Numerical Relativity
Conference, Golm, July 200
Nonequilibrium dynamics of a simple stochastic model
We investigate the low-temperature dynamics of a simple stochastic model,
introduced recently in the context of the physics of glasses. The slowest
characteristic time at equilibrium diverges exponentially at low temperature.
On smaller time scales, the nonequilibrium dynamics of the system exhibits an
aging regime. We present an analytical study of the scaling behaviour of the
mean energy, of its local correlation and response functions, and of the
associated fluctuation-dissipation ratio throughout the regime of low
temperature and long times. This analysis includes the aging regime, the
convergence to equilibrium, and the crossover behaviour between them.Comment: 36 pages, plain tex, 7 figures, to be published by Journal of Physics
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