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
Yeates A
(2011)
A generalized flux function for three-dimensional magnetic reconnection
in Physics of Plasmas
Yeates A
(2013)
Unique topological characterization of braided magnetic fields
in Physics of Plasmas
Yeates A
(2013)
Kinematic active region formation in a three-dimensional solar dynamo model
in Monthly Notices of the Royal Astronomical Society
Yeates A
(2011)
Dynamical constraints from field line topology in magnetic flux tubes
in Journal of Physics A: Mathematical and Theoretical
Yeates A
(2012)
Lagrangian coherent structures in photospheric flows and their implications for coronal magnetic structure
in Astronomy & Astrophysics
Yeates A
(2010)
Solar Cycle Variation of Magnetic Flux Ropes in a Quasi-Static Coronal Evolution Model
in Solar Physics
Yeates A
(2014)
The coronal energy input from magnetic braiding
in Astronomy & Astrophysics
Yeates A
(2013)
Coronal Magnetic Field Evolution from 1996 to 2012: Continuous Non-potential Simulations
in Solar Physics
Yeates AR
(2010)
Topological constraints on magnetic relaxation.
in Physical review letters
Zaqarashvili T
(2010)
Oscillations and Waves in Solar Spicules
in Space Science Reviews
Zhang K
(2013)
The non-resonant response of fluid in a rapidly rotating sphere undergoing longitudinal libration
in Journal of Fluid Mechanics
ZHANG K
(2009)
The onset of convection in rotating circular cylinders with experimental boundary conditions
in Journal of Fluid Mechanics
Zhang K
(2010)
On fluid flows in precessing spheres in the mantle frame of reference
in Physics of Fluids
ZHANG K
(2011)
On fluid motion in librating ellipsoids with moderate equatorial eccentricity
in Journal of Fluid Mechanics
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 |