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
(2009)
Bistability and hysteresis of dipolar dynamos generated by turbulent convection in rotating spherical shells
in EPL (Europhysics Letters)
Busse F
(2011)
Remarks on some typical assumptions in dynamo theory
in Geophysical & Astrophysical Fluid Dynamics
Berkoff N
(2010)
Comparison of the anelastic approximation with fully compressible equations for linear magnetoconvection and magnetic buoyancy
in Geophysical & Astrophysical Fluid Dynamics
Liao X
(2009)
Inertial oscillation, inertial wave and initial value problem in rotating annular channels
in Geophysical & Astrophysical Fluid Dynamics
Botha G
(2012)
Formation of magnetic flux tubes in cylindrical wedge geometry
in Geophysical & Astrophysical Fluid Dynamics
Mizerski K
(2012)
Large-scale convective dynamos in a stratified rotating plane layer
in Geophysical & Astrophysical Fluid Dynamics
Mizerski K
(2011)
The effect of stratification and compressibility on anelastic convection in a rotating plane layer
in Geophysical & Astrophysical Fluid Dynamics
Bushby P
(2012)
Convectively driven dynamo action in the quiet Sun
in Geophysical & Astrophysical Fluid Dynamics
Ji Y
(2014)
Asymptotic solutions for mean-field slab dynamos
in Geophysical & Astrophysical Fluid Dynamics
Brummell N
(2010)
Dynamo efficiency in compressible convective dynamos with and without penetration
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 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 |