Parallel computing resources for the UK MHD community

Lead Research Organisation: University of Leeds
Department Name: Applied Mathematics


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.


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Arber T (2009) THERMAL FRONTS IN FLARING MAGNETIC LOOPS in The Astrophysical Journal

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Barkov M (2010) Close binary progenitors of gamma-ray bursts in Monthly Notices of the Royal Astronomical Society

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Botha G (2010) Thermal conduction effects on the kink instability in coronal loops in Astronomy & Astrophysics

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Bowker J (2014) Incorporating velocity shear into the magneto-Boussinesq approximation in Geophysical & Astrophysical Fluid Dynamics

Description The computations carried out with this equipment has shown us how magnetic fields play a crucial role in many astrophysical objects such as stars, accretion discs and galaxies.
Exploitation Route Our work has stimulated others to use many of our computational techniques to study astrophysical magnetic fields.
Sectors Aerospace, Defence and Marine,Energy,Environment

Description The numerical methods that have been developed during the project have been used in and industrial application: safety assessment of liquid carbon dioxide transport.
First Year Of Impact 2012
Sector Aerospace, Defence and Marine,Energy,Environment
Impact Types Cultural,Economic