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.
The MPS is one of the leading institutes worldwide in building instruments for solar research, both for ground based observatories as well as for balloon and space-borne missions. Scientists and engineers of MPS conceive new observing methods and develop novel instruments of highest technological complexity. These instruments are built in house, tested, calibrated, and used at the best solar observatories in the world, or delivered to NASA and ESA to be launched to space.
The magnetic field in the solar atmosphere exceeds the geomagnetic field strength by four orders of magnitude. It greatly influences the processes of energy transport within the solar atmosphere, and dominates the morphology of the solar chromosphere and corona. Kinetic energy from convective motions in the Sun can be efficiently stored in magnetic fields and subsequently released - to heat the solar corona to several million degrees or to blast off coronal mass ejections.
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.
In the "Solar and Stellar Interiors" department, Laurent Gizon, Tom Duvall, Jesper Schou, Aaron Birch, Robert Cameron, Friedrich Kupka 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.
PhD project(s) would either focus on (1) the data acquisition and data analysis of atmospheres of planets and their moons, (2) the improvement or development of radiative transfer codes, models and simulations for the analysis of the data, (3) the development of sophisticated instrumentation.
The Solar and Stellar Coronae group employs spectroscopic, imaging, and stereoscopic techniques to analyse observations from extreme UV solar telescopes and coronagraphs. On the side of theory and (numerical) simulations we use magnetic modelling to extrapolate magnetic fields and 3D magneto-static and magneto-hydrodynamic models.