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
Hughes D
(2011)
The a-effect in rotating convection: a comparison of numerical simulations
in Monthly Notices of the Royal Astronomical Society: Letters
Botha G
(2011)
CHROMOSPHERIC RESONANCES ABOVE SUNSPOT UMBRAE
in The Astrophysical Journal
Galsgaard K
(2011)
Current accumulation at an asymmetric 3D null point caused by generic shearing motions
in Astronomy & Astrophysics
Jones C
(2011)
Planetary Magnetic Fields and Fluid Dynamos
in Annual Review of Fluid Mechanics
Favier B
(2011)
Small-scale dynamo action in rotating compressible convection
in Journal of Fluid Mechanics
Tsiklauri D
(2011)
Galaxy rotation curves: the effect of $\vec{j} \times\vec{B}$ force
in Astrophysics and Space Science
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
Bareford M
(2011)
The Flare-Energy Distributions Generated by Kink-Unstable Ensembles of Zero-Net-Current Coronal Loops
in Solar Physics
Fedun V
(2011)
MHD waves generated by high-frequency photospheric vortex motions
in Annales Geophysicae
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 |