The Sun has always been a unique source for our understanding of the Universe in its many forms. It provides a working example where both magnetic and non-magnetic structures can be studied over an enormous range of spatial (100 km – 100,000 km) and temporal (subsecond to months) scales. While we are only able to catch glimpses of these processes and phenomena in other astrophysical sources, the Sun provides a vantage reference point where the complex interplay between the plasma and the magnetic field is visible and can be studied continuously with unprecedented detail. The temperature in the Sun’s outer atmosphere rises rapidly from a few thousand degrees in the photosphere to over one million in the corona. Understanding how the Sun manages to achieve this feat requires an accurate evaluation of the magnetic field annihilation processes and the conversion of magnetic energy into heat.
The brightness and spectrum of the solar atmosphere are two very common properties used in most research studies. However, there exist a third property: polarisation. Polarisation is as important as brightness and an essential property of light that can be used as a diagnostic for the magnetic field. Dedicated instruments have been constructed that measure the Stokes profiles of spectral lines with high polarimetric accuracy and sensitivity. State-of-the-art inversion techniques have been developed alongside the instruments to extract physical information from spectropolarimetric observations.
The main aims of the project can be summarized as follows:
The student will use observations from state-of-the-art solar facilities in Europe and US. He/she will work in collaboration with researchers within QUB and other research institutes.
NICOLE+RH, HAZEL (Inversion algorithms), Swedish Solar Telescope (La Palma), Dunn Solar Telescope (New Mexico), Daniel K Inoue Solar Telescope (Maui), GREGOR Telescope (Tenerife)
More information from the primary supervisor: Prof Mihalis Mathioudakis (Email: email@example.com)