Solar and Magnetospheric Plasma Theory

The Solar and Magnetospheric Theory Group (SMTG) of the University of St Andrews will work on the fundamental physical processes occurring in the Sun's atmosphere and planetary magnetospheres. For example:
i) How do sunspots form, evolve and decay? ii) Why is the Sun's outer atmosphere (the corona) over 100 times hotter than the visible surface of the Sun so that the gas is ionized and forms a plasma? iii) What causes the waves in the Sun's atmosphere and what can these waves tell us about the local conditions there? iv) How does the Sun's magnetic field evolve over days, months and years and how does it interact with the Earth? v) How are electrons accelerated during solar magnetic disturbances? vi) How do solar magnetic fields interact with each other?
The answers to many of these key questions depend upon a range of expertise and the SMTG is in an excellent position to answer these questions.
We study a wide variety of physical phenomena using mathematical modelling (a combination of fundamental theory, analytical models, computer simulations, forward modelling and observations). It is an integrated approach that is needed, i.e. a mixture of modelling methods and a comparison between observations from several satellite missions and the theoretical models. The topics we will investigate, using plasma theory, are: i) the emergence of new magnetic field from the solar interior, the formation and evolution of active regions, the formation of cool dense prominences and the evolution of the global magnetic field of the Sun, ii) the physical mechanisms through which magnetic fields break their connectivity, reconnect with neighbouring fieldlines and how particles are accelerated to high speeds, iii) the use of Magnetohydrodynamics (MHD) wave theory to deduce properties of the solar atmosphere and magnetic field (coronal seismology), iv) the physical mechanisms responsible for keeping the corona much hotter than the lower parts of the solar atmosphere (coronal heating), v) the coupling of the 3 distinct magnetospheric MHD waves and the physics of the coupling of planetary magnetospheres to their ionospheres. These phenomena obey physical laws that can be expressed as non-linear partial differential equations. However, what makes them distinct is that different phenomena require different dominant terms. Hence, the physical processes and the plasma response will be different in each case. For example, magnetic reconnection requires electrical resistance but MHD waves in general do not. Gravity is important in flux emergence and prominence formation, but for magnetic reconnection it is not. Particle acceleration in solar flares and the magnetosphere requires a kinetic (particle) description, while many of the others research areas do not. It is the rich complexity of the non-linear equations that makes them hard to solve and to determine what the key physical processes are responsible for each event.
A most important research tool is the parallel computer formed by linking many commodity processors together. Then the simulation involves splitting the problem up into smaller parts that run on different processors at the same time (in parallel). Thus, our simulations are completed quicker. Hence, with a job that would require 10 years on single machine, will be completed in a couple of weeks on 512 processors.
We address key issues in the STFC Science Roadmap, especially, how does the Sun affect the Earth? However, a detailed understanding of the physics of our research topics are important not only for the Sun, solar-like stars and space weather, but also for understanding such diverse astrophysical processes such as star formation in giant molecular clouds, the evolution of astrophysical discs around stars, black holes and in Active Galactic Nuclei, and the physics of winds and outflows from stellar to extragalactic scales.

While the main impact of the proposed research will undoubtedly be of academic in nature, there will also be significant economic and societal impact. The skills required for research in theoretical solar physics means that our group is continually producing people skilled in mathematical modelling, computational (including parallel computing) methods, visualisation techniques and logical thinking for non-academic professions. While nearly 40 former group members have gone on to academic positions, over 50 former group members have flourishing careers outside academia. Thus, we are enhancing the research capacity, knowledge and skills of businesses and organisations. Several former PhD students have joined the Atomic Weapons Establishment (Aldermaston) and GCHQ, potentially improving national security.

Our public lectures and presentations at various science fairs, for example during the International Heliospheric Year, have helped to increase public awarness in the importance of our research. Our visits to both primary and secondary schools have helped to enthuse students to study science, in general, and physics and mathematics, in particular. The Space Camp and Sutton Trust summer schools are particularly popular with primary and secondary pupils. The Sun-Trek and History of Mathematics websites are fantastic online resources that appeal to both children and the wider public.

On the academic impact front, we have organised many conferences over the years and will be organising the major meetings, Hinode 6 in August 2012 and NAM 2013. We propose organising an HPC workshop for new UK MHD PhD students who will be using the UKMHD Consortium facilities for their research.