Smitha, H. N.; Anusha, L. S.; Solanki, S. K.; Riethmueller, T. L.: Flux emergence rate in the quiet Sun from SUNRISE data. SOLARNET IV, The Physics of the Sun from the Interior to the Outer Atmosphere, Lanzarote, Spain (2017)
In the "Solar and Stellar Interiors" department, Laurent Gizon, Jesper Schou, Aaron Birch, Robert Cameron and others offer PhD projects in solar physics and astrophysics. Helioseismology and asteroseismology are used as important tools to study the oscillating Sun and stars.
Recently new, very sensitive observations of the ExoMars Trace Gas Orbiter (TGO) and its instruments NOMAD (Nadir and Occultation for MArs Discovery) an ACS (Atmospheric Chemistry Suite) became available and initiated a number of interesting scientific questions. Some of them are open PhD projects using the MPS General Circulation Model (MPS-GCM).
The Solar Lower Atmosphere and Magnetism (SLAM) group covers many exciting subjects in solar physics, focussing on the development and testing of highly novel solar instrumentation, reduction and analysis of highest quality solar observations, or improving and developing advanced techniques for the analysis of solar observations.
Turbulence plays a very important role in many applications, ranging from geophysics and astrophysics to engineering. In our solar system, turbulence is often driving by thermal effect, rotation, and magnetic field. In this project you will use high-fidelity simulation tools, including direct numerical simulations, data assimilation, and machine learning, to study the physics of turbulence, focusing on convection and dynamos.
The Planetary Plasma Environments group (PPE) has a strong heritage in the exploration of planetary magnetospheres and space plasma interactions throughout the solar system. It has contributed instruments to several past missions that flew-by or orbited Jupiter (Galileo, Cassini, Ulysses). The PPE participates in the JUICE mission by contributing hardware and scientific expertise to the Particle Environment Package (PEP).
Inversion codes are used to aid the detailed interpretation of solar spectro-polarimetric data. This computer code attempts to find the atmospheric structure that produced an observed spectrum by minimizing the difference between the observed spectrum and a Stokes spectrum.