Parallel Computing Resources for the UK MHD Community
Lead Research Organisation:
University of St Andrews
Department Name: Mathematics and Statistics
Abstract
Virtually all material in the universe consists of an ionised gas called a plasma. Plasmas conduct electricity and interact with magnetic fields, producing many physical phenomena not easily reproduced in laboratories on Earth. The large-scale behaviour of these plasmas can be predicted by using a known set of complicated mathematical equations, called the equations of Magnetohydrodynamics (MHD). The solutions of MHD equations can describe the behaviour of plasmas in which collisions dominate the physical processes, such as (i) the generation of magnetic fields through a process known as dynamo action, (ii) the release of a staggering amount of magnetic energy in a large solar flare by magnetic reconnection, (iii) the small scale chaotic motions of turbulence in a magnetised plasma, (iv) the fact that solar atmosphere is much hotter than the solar surface and (v) the way in which gigantic eruptions of solar plasma interact with the Earth's magnetic field to produce the Aurora. When collisional effects are weak, in low-density plasmas and in problems involving short length-scales, the more fundamental kinetic equations must be solved. However, the solution of both sets of equations require extremely large computers and the best way is to link several hundred computers together and get them all working on a fraction of the large problem. These computers are called parallel computers. The UK effort in this research area is at the forefront of the worldwide effort to understand how the Sun, the Solar System and astrophysical plasmas work. While this work is essentially theoretical, it is driven by the observations of the present fleet of solar and astrophysical ground and space-based observatories.
Organisations
Publications
Sreenivasan B
(2011)
Helicity generation and subcritical behaviour in rapidly rotating dynamos
in Journal of Fluid Mechanics
Busse F
(2011)
Remarks on some typical assumptions in dynamo theory
in Geophysical & Astrophysical Fluid Dynamics
Favier B
(2011)
Small-scale dynamo action in rotating compressible convection
in Journal of Fluid Mechanics
Mizerski K
(2011)
The effect of stratification and compressibility on anelastic convection in a rotating plane layer
in Geophysical & Astrophysical Fluid Dynamics
Tsiklauri D
(2011)
Particle acceleration by circularly and elliptically polarised dispersive Alfven waves in a transversely inhomogeneous plasma in the inertial and kinetic regimes
in Physics of Plasmas
Galsgaard K
(2011)
Steady state reconnection at a single 3D magnetic null point
in Astronomy & Astrophysics
Botha G
(2011)
CHROMOSPHERIC RESONANCES ABOVE SUNSPOT UMBRAE
in The Astrophysical Journal
MacTaggart D
(2011)
Flux emergence within mature solar active regions
in Astronomy & Astrophysics
Gordovskyy M
(2011)
PARTICLE ACCELERATION BY MAGNETIC RECONNECTION IN A TWISTED CORONAL LOOP
in The Astrophysical Journal
Gruszecki M
(2011)
Slow magnetacoustic waves in magnetic arcades
in Astronomy & Astrophysics
Pontin D
(2011)
Three-dimensional magnetic reconnection regimes: A review
in Advances in Space Research
Liang Y
(2011)
Observations of multi-resonance effect in ELM control with magnetic perturbation fields on the JET tokamak
in Nuclear Fusion
Houghton S
(2011)
Localized plumes in three-dimensional compressible magnetoconvection Localized plumes in magnetoconvection
in Monthly Notices of the Royal Astronomical Society
Pontin D
(2011)
Generalised models for torsional spine and fan magnetic reconnection
in Astronomy & Astrophysics
Tsiklauri D
(2011)
An alternative to the plasma emission model: Particle-in-cell, self-consistent electromagnetic wave emission simulations of solar type III radio bursts
in Physics of Plasmas
Gruszecki M
(2011)
Magnetoacoustic shock formation near a magnetic null point
in Astronomy & Astrophysics
Galsgaard K
(2011)
Current accumulation at an asymmetric 3D null point caused by generic shearing motions
in Astronomy & Astrophysics
Yeates A
(2011)
A generalized flux function for three-dimensional magnetic reconnection
in Physics of Plasmas
Tobias S
(2011)
ASTROPHYSICAL FLUID DYNAMICS VIA DIRECT STATISTICAL SIMULATION
in The Astrophysical Journal
Bareford M
(2011)
The Flare-Energy Distributions Generated by Kink-Unstable Ensembles of Zero-Net-Current Coronal Loops
in Solar Physics
Botha G
(2012)
Formation of magnetic flux tubes in cylindrical wedge geometry
in Geophysical & Astrophysical Fluid Dynamics
Simitev R
(2012)
HOW FAR CAN MINIMAL MODELS EXPLAIN THE SOLAR CYCLE?
in The Astrophysical Journal
Pontin D
(2012)
ON THE FORMATION OF CURRENT SHEETS IN RESPONSE TO THE COMPRESSION OR EXPANSION OF A POTENTIAL MAGNETIC FIELD
in The Astrophysical Journal
Bushby P
(2012)
Convectively driven dynamo action in the quiet Sun
in Geophysical & Astrophysical Fluid Dynamics
Moschou S
(2012)
SDO Observations of Solar Jets
in Solar Physics
| Description | The computations carried out with this equipment has shown us how magnetic fields play a crucial role in many astrophysical objects such as the Sun, stars, accretion discs and galaxies. |
| Exploitation Route | The research results will be used to extend our knowledge and suggest new areas for research. Our work has stimulated others to use many of our computational techniques in other areas of research. |
| Sectors | Education Other |