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
Simitev R
(2012)
HOW FAR CAN MINIMAL MODELS EXPLAIN THE SOLAR CYCLE?
in The Astrophysical Journal
Simitev R
(2009)
Bistability and hysteresis of dipolar dynamos generated by turbulent convection in rotating spherical shells
in EPL (Europhysics Letters)
Silvers L
(2009)
Interactions between magnetohydrodynamic shear instabilities and convective flows in the solar interior
in Monthly Notices of the Royal Astronomical Society
Shelyag S
(2009)
Acoustic wave propagation in the solar sub-photosphere with localised magnetic field concentration: effect of magnetic tension
in Astronomy & Astrophysics
Scullion E
(2009)
JETS IN POLAR CORONAL HOLES
in The Astrophysical Journal
Schrijver C
(2013)
PATHWAYS OF LARGE-SCALE MAGNETIC COUPLINGS BETWEEN SOLAR CORONAL EVENTS
in The Astrophysical Journal
Schmitz H
(2013)
The effect of initial conditions on the electromagnetic radiation generation in type III solar radio bursts
in Physics of Plasmas
Russell A
(2013)
Production of small-scale Alfvén waves by ionospheric depletion, nonlinear magnetosphere-ionosphere coupling and phase mixing
in Journal of Geophysical Research: Space Physics
Russell A
(2013)
Solar flares and focused energy transport by MHD waves
in Astronomy & Astrophysics
Russell A
(2013)
PROPAGATION OF ALFVÉNIC WAVES FROM CORONA TO CHROMOSPHERE AND CONSEQUENCES FOR SOLAR FLARES
in The Astrophysical Journal
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 |