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My project is to model the Solar dynamo with fully compressible resistive magnetohydrodynamics (MHD) using the Pencil Code in high performance parallel numerical computations. The dynamics of the Sun are critically dependent on the strong magnetic fields it generates within its interior by various dynamo processes. The interaction betwenn the magnetic field and the highly turbulent hot plasma comprising the Sun, lead to variations in radiation and intermittent explosive events, which may sporadically shower the Earth with bursts of high energy particles, which can be critical to power grids, aircraft and particularly to space craft. In addition there may also be consequences for the long term and short term variability of terrestrial temperatures.
There are many aspects of these processes, which are poorly understood, such as the structure and mechansim for the solar dynamo; the nature of heating of the solar atmosphere and causes and predictability of solar flares, solar wind and coronal mass ejections; the interaction between the solar wind, space weather and the planetary atmosphere and magnetic field, which protects us from the destructive power of the solar wind. Our group in Aalto is investigating the soalr dynamo, within the umbrella of the Academy of Finland Center of Excellence: Research on Solar Long-term Variability and Effects (ReSoLVE), alongside other groups considering other aspects of the process trhough the solar atmosphere, interplanetary space weather and the Earth's ionosphere.
My project is to model the Solar dynamo with fully compressible resistive magnetohydrodynamics (MHD) using the Pencil Code in high performance parallel numerical computations. The dynamics of the Sun are critically dependent on the strong magnetic fields it generates within its interior by various dynamo processes. The interaction betwenn the magnetic field and the highly turbulent hot plasma comprising the Sun, lead to variations in radiation and intermittent explosive events, which may sporadically shower the Earth with bursts of high energy particles, which can be critical to power grids, aircraft and particularly to space craft. In addition there may also be consequences for the long term and short term variability of terrestrial temperatures.
There are many aspects of these processes, which are poorly understood, such as the structure and mechansim for the solar dynamo; the nature of heating of the solar atmosphere and causes and predictability of solar flares, solar wind and coronal mass ejections; the interaction between the solar wind, space weather and the planetary atmosphere and magnetic field, which protects us from the destructive power of the solar wind. Our group in Aalto is investigating the soalr dynamo, within the umbrella of the Academy of Finland Center of Excellence: Research on Solar Long-term Variability and Effects (ReSoLVE), alongside other groups considering other aspects of the process trhough the solar atmosphere, interplanetary space weather and the Earth's ionosphere.
I originate from Newcastle upon Tyne, United Kingdom, native language (Geordie) English. I returned to education to take my undergaduate degree in mathematics (MMath First) at Newcastle University 2004-2008, followed by a Ph.D. in applied mathematics and astrophysics, also at Newcastle 2008-2012. My thesis "Supernova Driven Turbulence in the Interstellar Medium" concerned HPC modelling of the galactic dynamo, successfully implementing 3D multi-phase MHD numerical simulations of spiral galaxies with realisitc magnetic fields, temperature and density structure.
My previous employment was at Sheffield University School of Mathematics and Statistics, 2012-2015, where I was working on the Sun's coronal heating. The atmosphere above the solar surface is typically 1million degrees K, 100x the temperature at the surface. How it is possible that plasma further away from the heat source should be systmeatically hotter than the surface is not understood, and we were modelling the magnetic field network analytically and numerically, in order to investigate what heating mechanisms might exist to explain this phenomena.
I originate from Newcastle upon Tyne, United Kingdom, native language (Geordie) English. I returned to education to take my undergaduate degree in mathematics (MMath First) at Newcastle University 2004-2008, followed by a Ph.D. in applied mathematics and astrophysics, also at Newcastle 2008-2012. My thesis "Supernova Driven Turbulence in the Interstellar Medium" concerned HPC modelling of the galactic dynamo, successfully implementing 3D multi-phase MHD numerical simulations of spiral galaxies with realisitc magnetic fields, temperature and density structure.
My previous employment was at Sheffield University School of Mathematics and Statistics, 2012-2015, where I was working on the Sun's coronal heating. The atmosphere above the solar surface is typically 1million degrees K, 100x the temperature at the surface. How it is possible that plasma further away from the heat source should be systmeatically hotter than the surface is not understood, and we were modelling the magnetic field network analytically and numerically, in order to investigate what heating mechanisms might exist to explain this phenomena.
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