53 research outputs found
Dynamical evolution of massive black holes in galactic-scale N-body simulations - Introducing the regularized tree code 'rVINE'
We present a hybrid code combining the OpenMP-parallel tree code VINE with an
algorithmic chain regularization scheme. The new code, called "rVINE", aims to
significantly improve the accuracy of close encounters of massive bodies with
supermassive black holes in galaxy-scale numerical simulations. We demonstrate
the capabilities of the code by studying two test problems, the sinking of a
single massive black hole to the centre of a gas-free galaxy due to dynamical
friction and the hardening of a supermassive black hole binary due to close
stellar encounters. We show that results obtained with rVINE compare well with
NBODY7 for problems with particle numbers that can be simulated with NBODY7. In
particular, in both NBODY7 and rVINE we find a clear N-dependence of the binary
hardening rate, a low binary eccentricity and moderate eccentricity evolution,
as well as the conversion of the galaxy's inner density profile from a cusp to
a a core via the ejection of stars at high velocity. The much larger number of
particles that can be handled by rVINE will open up exciting opportunities to
model stellar dynamics close to SMBHs much more accurately in a realistic
galactic context. This will help to remedy the inherent limitations of commonly
used tree solvers to follow the correct dynamical evolution of black holes in
galaxy scale simulations
Star Clusters
This review concentrates almost entirely on globular star clusters. It
emphasises the increasing realisation that few of the traditional problems of
star cluster astronomy can be studied in isolation: the influence of the Galaxy
affects dynamical evolution deep in the core, and the spectrum of stellar
masses; in turn the evolution of the core determines the highest stellar
densities, and the rate of encounters. In this way external tidal effects
indirectly influence the formation and evolution of blue stragglers, binary
pulsars, X-ray sources, etc. More controversially, the stellar density appears
to influence the relative distribution of normal stars. In the opposite sense,
the evolution of individual stars governs much of the early dynamics of a
globular cluster, and the existence of large numbers of primordial binary stars
has changed important details of our picture of the dynamical evolution. New
computational tools which will become available in the next few years will help
dynamical theorists to address these questions.Comment: 10 pages, 3 figures, Te
Improving the scalability of parallel N-body applications with an event driven constraint based execution model
The scalability and efficiency of graph applications are significantly
constrained by conventional systems and their supporting programming models.
Technology trends like multicore, manycore, and heterogeneous system
architectures are introducing further challenges and possibilities for emerging
application domains such as graph applications. This paper explores the space
of effective parallel execution of ephemeral graphs that are dynamically
generated using the Barnes-Hut algorithm to exemplify dynamic workloads. The
workloads are expressed using the semantics of an Exascale computing execution
model called ParalleX. For comparison, results using conventional execution
model semantics are also presented. We find improved load balancing during
runtime and automatic parallelism discovery improving efficiency using the
advanced semantics for Exascale computing.Comment: 11 figure
A spatially-structured PCG method for content diversity in a Physics-based simulation game
This paper presents a spatially-structured evolutionary algorithm (EA) to procedurally generate game maps of di ferent levels of di ficulty to be solved, in Gravityvolve!, a physics-based simulation videogame that we have implemented and which is inspired by the n-
body problem, a classical problem in the fi eld of physics and mathematics. The proposal consists of a steady-state EA whose population is partitioned into three groups according to the di ficulty of the generated content (hard, medium or easy) which can be easily adapted to handle the automatic creation of content of diverse nature in other games. In addition, we present three fitness functions, based on multiple criteria (i.e:, intersections, gravitational acceleration and simulations), that were used experimentally to conduct the search process for creating a database of
maps with di ferent di ficulty in Gravityvolve!.Universidad de Málaga. Campus de Excelencia Internacional AndalucĂa Tech
The inevitable youthfulness of known high-redshift radio galaxies
Radio galaxies can be seen out to very high redshifts, where in principle
they can serve as probes of the early evolution of the Universe. Here we show
that for any model of radio-galaxy evolution in which the luminosity decreases
with time after an initial rapid increase (that is, essentially all reasonable
models), all observable high-redshift radio-galaxies must be seen when the
lobes are less than 10^7 years old. This means that high-redshift radio
galaxies can be used as a high-time-resolution probe of evolution in the early
Universe. Moreover, this result helps to explain many observed trends of
radio-galaxy properties with redshift [(i) the `alignment effect' of optical
emission along radio-jet axes, (ii) the increased distortion in radio
structure, (iii) the decrease in physical sizes, (iv) the increase in radio
depolarisation, and (v) the increase in dust emission] without needing to
invoke explanations based on cosmology or strong evolution of the surrounding
intergalactic medium with cosmic time, thereby avoiding conflict with current
theories of structure formation.Comment: To appear in Nature. 4 pages, 2 colour figures available on request.
Also available at http://www-astro.physics.ox.ac.uk/~km
Binaries and Globular Cluster Dynamics
We summarize the results of recent theoretical work on the dynamical
evolution of globular clusters containing primordial binaries. Even a very
small initial binary fraction (e.g., 10%) can play a key role in supporting a
cluster against gravothermal collapse for many relaxation times. Inelastic
encounters between binaries and single stars or other binaries provide a very
significant energy source for the cluster. These dynamical interactions also
lead to the production of large numbers of exotic systems such as ultracompact
X-ray binaries, recycled radio pulsars, double degenerate systems, and blue
stragglers. Our work is based on a new parallel supercomputer code implementing
Henon's Monte Carlo method for simulating the dynamical evolution of dense
stellar systems in the Fokker-Planck approximation. This new code allows us to
calculate very accurately the evolution of a cluster containing a realistic
number of stars (N ~ 10^5 - 10^6) in typically a few hours to a few days of
computing time. The discrete, star-by-star representation of the cluster in the
simulation makes it possible to treat naturally a number of important
processes, including single and binary star evolution, all dynamical
interactions of single stars and binaries, and tidal interactions with the
Galaxy.Comment: 15 pages, to appear in `The Influence of Binaries on Stellar
Population Studies', ed. D. Vanbeveren (Kluwer
The formation of massive black holes through collision runaway in dense young star clusters
A luminous X-ray source is associated with a cluster (MGG-11) of young stars
\~200pc from the center of the starburst galaxy M82. The properties of the
X-ray source are best explained by a black hole with a mass of at least
350Msun, which is intermediate between stellar-mass and supermassive black
holes. A nearby but somewhat more massive star cluster (MGG-9) shows no
evidence of such an intermediate mass black hole, raising the issue of just
what physical characteristics of the clusters can account for this difference.
Here we report numerical simulations of the evolution and the motions of stars
within the clusters, where stars are allowed to mergers with each other. We
find that for MGG-11 dynamical friction leads to the massive stars sinking
rapidly to the center of the cluster to participate in a runaway collision,
thereby producing a star of 800-3000Msun, which ultimately collapses to an
black hole of intermediate mass. No such runaway occurs in the cluster MGG-9
because the larger cluster radius leads to a mass-segregation timescale a
factor of five longer than for MGG-11.Comment: Accepted for publication in Nature (Including supplementary
information
The stellar and sub-stellar IMF of simple and composite populations
The current knowledge on the stellar IMF is documented. It appears to become
top-heavy when the star-formation rate density surpasses about 0.1Msun/(yr
pc^3) on a pc scale and it may become increasingly bottom-heavy with increasing
metallicity and in increasingly massive early-type galaxies. It declines quite
steeply below about 0.07Msun with brown dwarfs (BDs) and very low mass stars
having their own IMF. The most massive star of mass mmax formed in an embedded
cluster with stellar mass Mecl correlates strongly with Mecl being a result of
gravitation-driven but resource-limited growth and fragmentation induced
starvation. There is no convincing evidence whatsoever that massive stars do
form in isolation. Various methods of discretising a stellar population are
introduced: optimal sampling leads to a mass distribution that perfectly
represents the exact form of the desired IMF and the mmax-to-Mecl relation,
while random sampling results in statistical variations of the shape of the
IMF. The observed mmax-to-Mecl correlation and the small spread of IMF
power-law indices together suggest that optimally sampling the IMF may be the
more realistic description of star formation than random sampling from a
universal IMF with a constant upper mass limit. Composite populations on galaxy
scales, which are formed from many pc scale star formation events, need to be
described by the integrated galactic IMF. This IGIMF varies systematically from
top-light to top-heavy in dependence of galaxy type and star formation rate,
with dramatic implications for theories of galaxy formation and evolution.Comment: 167 pages, 37 figures, 3 tables, published in Stellar Systems and
Galactic Structure, Vol.5, Springer. This revised version is consistent with
the published version and includes additional references and minor additions
to the text as well as a recomputed Table 1. ISBN 978-90-481-8817-
Development of the Adolescent Preoccupation with Screens Scale
Abstract Background Although public health concerns have been raised regarding the detrimental health effects of increasing rates of electronic screen use among adolescents, such effects have been small. Instruments currently available tend to be lengthy, have a clinical research focus, and assess young people’s screen use on specific screen-based activities (e.g., TV, computer, or internet). None appear to address screen use across a broad range of screens, including mobile devices and screen-based activities. The objective was to develop a new and short self-report scale for investigating adolescents’ screen use across all screens and screen-based activities in non-clinical settings. Methods The Adolescent Preoccupation with Screens Scale (APSS) was developed over a three stage process. First, a review of the current literature and existing instruments was undertaken and suitable items identified. Second, the draft APSS was piloted with adolescents and item affectivity and discrimination indices were calculated. Third, a cross sectional school based online survey of 1967 Australian adolescents in grades 5 (10 years old), 7 (13 years) and 9 (15 years) from 25 randomly selected schools was conducted. Results Factor Analysis on a sub-sample of the data (n = 782) and Confirmatory Factor Analysis on the remaining sub-sample (n = 1185), supported a two-factor model. The first factor reflects adolescents’ mood management with screen use, and the second reflects a behavioural preoccupation. The measure demonstrated strong invariance across sex and across Grades 5, 7, and 9. Both factors displayed good internal consistency (α = .91 and .87, respectively). Sex and grade differences on both scales were investigated and boys in Grade 5 reported higher levels of both mood management and behavioural preoccupation with screens. There were no sex differences on mood management in Grades 7 and 9, but girls reported higher behavioural preoccupation in both these later grades. Conclusion The APSS provides researchers with a new, brief and robust measure of potentially problematic screen use across a wide array of screens, including mobile devices, so readily accessed during adolescence
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