Applied Mathematics Seminars: Numerical Modelling of the Solar Interior and Lower Atmosphere: Bridging Theory and Observations
27 January 2017 14:00 in CM219
Computational modelling occupies a significant niche in solar physics, in part due to its ability to link physical processes in the solar interior, invisible for an observer, to their observable counterparts in the solar atmosphere. Furthermore, numerical simulations allow us to compute the details of solar radiation (intensity, polarisation), thus providing a unique possibility to understand, analyse and sometimes even predict dynamical behaviour of waves, flows and magnetic fields in the interconnected solar interior and atmosphere. Due to their intrinsic expandability, numerical simulations aim at solving more complex physical problems, compared to the purely analytical approach, and are, probably, the key to the solution of the long-standing problem of the energy transport through the solar atmosphere.
In my seminar, I will present a range of magneto-hydrodynamic simulations of interconnected solar interior and atmosphere with different levels of realism. Using a solar radiative magneto-convection model, I will demonstrate presence of a large amount of energy in Alfvén waves, naturally generated by convective photospheric motions. These waves may be responsible for creation of the solar atmospheric temperature profile and, ultimately, for energy transport through the solar atmosphere. I will show our recent simulations of magneto-hydrodynamic wave propagation and absorption through the partially-ionised solar atmosphere and will discuss the mechanisms for the chromospheric Alfvén wave absorption. Finally, I will demonstrate the presence of line profiles with both emission and absorption features at the simulated solar limb, and pure emission profiles above the limb, and discuss physical origins of the emission wings in the Stokes profiles at the limb, their possible link to spicules and solar atmospheric Alfvén waves.
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