Mr
Justus Tobias Tsang
(University of Southampton)
08/09/2016, 12:45
Poster
I will present the status of RBC/UKQCDs charmed meson decay constant study. I will also highlight RBC/UKQCDs wider charm physics program and outline current studies.
Mr
Andrea Cristini
(Keele University)
08/09/2016, 12:45
Poster
Stellar models are important for many areas of astrophysics, for example nucleosynthesis yields, supernova progenitor models and understanding physics at extreme conditions. One of the longest standing problems with stellar evolution models is the treatment of convection. To study convection and turbulent motions in stellar interiors, detailed 3D hydrodynamical simulations are...
Prof.
Paul Shellard
(University of Cambridge)
08/09/2016, 12:45
Poster
Poster describing the work of the Intel Parallel Computing Centre associated with the COSMOS@DiRAC SMP Facility hosted in Cambridge. This describes the unique hybrid architecture of the COSMOS system, including shared-memory capabilities and accelerators (Xenon Phi) and radical optimisations that have been undertaken for new many-core processors. Highlights include refactoring of the Modal...
Mr
Thomas Helfer
(Kings College London)
08/09/2016, 12:45
Poster
While static axis-symmetric solutions of gravitating cosmic strings have been found numerically, dynamical solutions are much harder propositions and little has been done in this aspect. We developed a solver for local U(1) together with Einstein field equations. Using the solutions of strings with perturbations from Vachaspati and Garfinkle, we find initial data for our string and construct...
Mr
Gerardo Ramon Fox
(University of St. Andrews)
08/09/2016, 12:45
Poster
F. G. Ramón Fox (1) and Ian Bonnell (1)
(1)University of St. Andrews
Galactic scale gas flows feed the growth of molecular clouds, the regions where stars form in high-density cores. These flows also play a role in driving the internal dynamics of these clouds, which affects their overall stability and star formation activity. The triggering of star formation involves a connection between...
Dr
Mark Richardson
(University of Oxford)
08/09/2016, 12:45
Poster
The circumgalactic medium (CGM) encompasses gas that extends from the outskirts of a galaxy to the edge of its halo, mediating gas accretion and outflows. Observations of absorption in background quasar spectra reveal a wealth of information about the structure of the CGM, in particular that it is an environment polluted by metals and cool gas from galactic outflows. By using simulations of...
Dr
Eugene Lim
(King's College London), Mr
Thomas Helfer
(Kings College London)
08/09/2016, 12:45
Poster
GRChombo is a new numerical relativity code specifically designed to efficiently and easily simulate the disparate length scales encountered in GR using fully adaptive mesh refinement and the latest parallel computing techniques. Applications range from gravitational wave signals produced from black hole mergers through to critical phenomena for high-dimensional black holes.
Dr
Azusa Yamaguchi
(Software Architect)
08/09/2016, 12:45
Poster
In this proceedings we discuss the motivation, implementation details, and performance of a new physics code base called Grid. It is intended to be more performant, more general, but similar in spirit to QDP++[ 6 ]. Our approach is to engineer the basic type system to be consistently fast, rather than bolt on a few optimised routines, and we are attempt to write all our optimised routines...
Dr
Nobuya Nishimura
(Keele University)
08/09/2016, 12:45
Poster
A variety of elements has been synthesised in the evolution of stars and supernovae since the Big-Bang. The thermonuclear nuclear reaction is the physical process responsible for the production of elements, and also drives nuclear-burnings in stellar interiors. We need to know accurate reaction rates to help understand the cosmic origin of elements. In our project, we try to identify “key”...
Mr
Sergio Martin-Alvarez
(University of Oxford)
08/09/2016, 12:45
Poster
Regardless of being acknowledged as a relevant factor in several astrophysical processes, the study of magnetic fields has been one of the most elusive areas of cosmology and galaxy evolution up to this day. The reason for it are both the complications associated with their observation and measurements, and the intricate difficulty to model them. However, the resources required to tackle them...
Prof.
Paul Shellard
(University of Cambridge)
08/09/2016, 12:45
Poster
We apply highly efficient modal methods (developed during the Planck analysis) to large-scale structure distributions in order to optimally evaluate the bispectrum in three dimensions. Currently, deployed on dark matter distributions from N-body codes, this tool is intended for estimating higher-order correlation functions from huge galaxy surveys like Euclid.
Mr
Felix Sainsbury-Martinez
(University of Exeter)
08/09/2016, 12:45
Poster
Low-Mass stars are typically fully convective, and as such their dynamics may differ significantly from sun-like stars. Here we present a series of 3D anelastic simulations of fully convective stars, designed to investigate how the meridional circulation, the differential rotation, and entropy are affected by varying stellar parameters, such as the luminosity or the rotation rate. We also...
Prof.
Peter Boyle
(Edinburgh)
08/09/2016, 12:45
Poster
We present a new class of multigrid solver algorithm suitable for the solution of 5d chiral fermions such as Domain Wall fermions and the Continued Fraction overlap. Unlike HDCG, arXiv:1402.2585, the algorithm works directly on a nearest neighbour fine operator. The fine operator used is Hermitian indefinite, for example Γ5Ddwf, and convergence is achieved with an indefinite matrix solver such...
Dr
Taysun Kimm
(KICC and IoA, University of Cambridge)
08/09/2016, 12:45
Poster
Reionisation in the early universe is likely driven by LyC photons from dwarf galaxies. Using high-resolution, cosmological radiation-hydrodynamic simulations, we study the escape of LyC photons from mini-haloes with the mass Mhalo < 1e8 Msun. Our simulations include a new thermo-turbulent star formation model, non-equilibrium photo-chemistry, and important stellar feedback processes...
Dr
Jonathan Chardin
(Institute of Astronomy (IOA) and Kavli Institute for Cosmology Cambridge (KICC), University of Cambridge)
08/09/2016, 12:45
Poster
Lyman-alpha forest data probing the post-reionization Universe shows surprisingly large opacity fluctuations over rather large ( 50 comoving Mpc/h) spatial scales.
We model these fluctuations using a hybrid approach utilizing the large volume Millennium simulation to predict the spatial distribution of QSOs combined with smaller scale full hydrodynamical simulation performed with RAMSES and...
Dr
Tom Goffrey
(University of Exeter)
08/09/2016, 12:45
Poster
Stellar evolution is influenced by a wide range of complex, multi-dimensional phenomena. The MUlti-dimensional Stellar Implicit Code, MUSIC, is a new code developed in Exeter with international collaborators that is designed to study such processes. MUSIC is a fully compressible, time-implicit code, which utilises realistic opacity and equation of state data, and is capable of simulating a...
Dr
Oliver Witzel
(University of Edinburgh)
08/09/2016, 12:45
Poster
In the Standard Model of elementary particle physics, b-quarks are the heaviest quarks forming hadronic bound states. Their large mass allows for many decay modes and by that tests of the Standard Model. Using numerical lattice QCD simulations we calculate decays of B-mesons, quark-antiquark pairs with one constituent a b-quark, into one other hadron and leptons. These calculations lead to...
Mr
Benjamin Lewis
(University of Exeter)
08/09/2016, 12:45
Poster
We expand on Lewis, et al. (2015) and (2016, submitted), which considered only ideal MHD simulations of the collapse of molecular cloud cores without turbulence, and use radiation magnetohydrodynamical calculations to explore how the physics of turbulence, rotation, magnetism and radiation influences the formation of protostars.
The inclusion of a flux limited diffusion radiative transfer...
Mr
James Willis
(ICC, Durham University)
08/09/2016, 12:45
Poster
SWIFT - Smoothed-Particle Hydrodynamics With Interdependent Fine-grained Tasking. We will describe the methods and techniques used to vectorise SWIFT and present the improvement to performance due to vectorisation.
Ms
Laura Keating
(Institute of Astronomy, University of Cambridge)
08/09/2016, 12:45
Poster
Observations of absorption lines in the spectra of QSOs out to redshift 7 provide an important probe of the intergalactic medium (IGM) at the tail end of reionization. In this talk I will discuss my work using high-resolution cosmological simulations to model the enrichment and ionization state of the high-redshift IGM. I will present results from cosmological simulations run with different...
Ms
Monique A. Henson
(Jodrell Bank Centre for Astrophysics, University of Manchester)
08/09/2016, 12:45
Poster
As the largest gravitationally bound structures in the Universe, galaxy clusters offer a crucial opportunity to study both the physics of structure formation and cosmology. There has been a wealth of work characterising the structure and properties of galaxy clusters in numerical simulations, however these have been focussed on dark matter only simulations or have been restricted to small...
Dr
Roger Horsley
(University of Edinburgh)
08/09/2016, 12:45
Poster
The proton consists of two valence up quarks, one
down quark together with a `sea' of quark anti-quark pairs
and gluons. How each constituent contributes to the
total spin of the proton has remained a mystery for many
years. In particular the quark contribution is much
smaller than expected. We discuss here our lattice QCD
determination of the quark contribution, using...
Dr
Rowan Smith
(University of Manchester)
08/09/2016, 12:45
Poster
We show how the AREPO code can be used to follow the ISM in spiral type galaxy simulations at unprecedented scales. The resolution extends from 6 kpc down to sub-pc scales and includes important physical processes such as supernova feedback, time-dependent chemistry and self-shielding, and gas self gravity. Such resolution means that we can resolve sub-structure within individual molecular...
