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
Gent F
(2013)
The supernova-regulated ISM - I. The multiphase structure
in Monthly Notices of the Royal Astronomical Society
Gent F
(2013)
The supernova-regulated ISM - II. The mean magnetic field
in Monthly Notices of the Royal Astronomical Society: Letters
Pontin DI
(2012)
Theory of magnetic reconnection in solar and astrophysical plasmas.
in Philosophical transactions. Series A, Mathematical, physical, and engineering sciences
Arber T
(2009)
THERMAL FRONTS IN FLARING MAGNETIC LOOPS
in The Astrophysical Journal
Tsiklauri D
(2012)
Three dimensional particle-in-cell simulation of particle acceleration by circularly polarised inertial Alfven waves in a transversely inhomogeneous plasma
in Physics of Plasmas
Pontin D
(2011)
Three-dimensional magnetic reconnection regimes: A review
in Advances in Space Research
Priest E
(2009)
Three-dimensional null point reconnection regimes
in Physics of Plasmas
Pechhacker R
(2014)
Three-dimensional particle-in-cell simulation of electron acceleration by Langmuir waves in an inhomogeneous plasma
in Physics of Plasmas
Yeates AR
(2010)
Topological constraints on magnetic relaxation.
in Physical review letters
Morton R
(2009)
TRANSVERSE OSCILLATIONS OF A COOLING CORONAL LOOP
in The Astrophysical Journal
Hughes DW
(2010)
Turbulent magnetic diffusivity tensor for time-dependent mean fields.
in Physical review letters
Dritschel D
(2012)
Two-dimensional magnetohydrodynamic turbulence in the small magnetic Prandtl number limit
in Journal of Fluid Mechanics
Yeates A
(2013)
Unique topological characterization of braided magnetic fields
in Physics of Plasmas
Tsiklauri D
(2010)
Vlasov - Maxwell, Self-consistent Electromagnetic Wave Emission Simulations in the Solar Corona
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 |