Dubinin, E. M.; Fränz, M.; Pätzold, M.; Tellmann, S.; Woch, J.; McFadden, J.; Zelenyi, L.: Bursty Ion Escape Fluxes at Mars. Journal of Geophysical Research: Space Physics 126 (4), e2020JA028920 (2021)
Dubinin, E. M.; Fränz, M.; Pätzold, M.; Woch, J.; McFadden, J.; Fan, K.; Wei, Y.; Tsareva, O.; Zelenyi, L.: Impact of Martian crustal magnetic field on the ion escape. Journal of Geophysical Research: Space Physics, e2020JA028010 (2020)
Dubinin, E. M.; Fränz, M.; Pätzold, M.; Woch, J.; McFadden, J.; Halekas, J. S.; Connerney, J. E. P.; Jakosky, B. M.; Eparvier, F.; Vaisberg, O.et al.; Zelenyi, L.: Expansion and Shrinking of the Martian Topside Ionosphere. Journal of Geophysical Research: Space Physics 124 (11), pp. 9725 - 9738 (2019)
Dubinin, E. M.; Modolo, R.; Fränz, M.; Päetzold, M.; Woch, J.; Chai, L.; Wei, Y.; Connerney, J. E. P.; Mcfadden, J.; DiBraccio, G.et al.; Espley, J.; Grigorenko, E.; Zelenyi, L.: The Induced Magnetosphere of Mars: Asymmetrical Topology of the Magnetic Field Lines. Geophysical Research Letters 46 (22), pp. 12722 - 12730 (2019)
Dubinin, E.; Fraenz, M.; Zhang, T. L.; Woch, J.; Wei, Y.: Magnetic fields in the Venus ionosphere: Dependence on the IMF direction‐ Venus Express observations. Journal Geophysical Research 119, pp. 7587 - 7600 (2014)
Dubinin, E.; Fraenz, M.; Zhang, T.-L.; Woch, J.; Wei, Y.; Fedorov, A.; Barabash, S.; R., L.: Plasma in the Near Venus Tail - Venus Express Observations. Journal Geophysical Research 118, pp. 7624 - 7634 (2013)
Dubinin, E.; Fraenz, M.; Woch, J.; Zhang, T.-L.; Wei, Y.; Fedorov, A.; Barabash, S.; R., L.: Toroidal and poloidal magnetic fields at Venus. Venus Express observations. Planetary and Space Science 87, pp. 19 - 29 (2013)
Dubinin, E.; Fraenz, M.; Woch, J.; Modolo, R.; Chanteur, G.; Duru, F.; Gurnett, D. A.; Barabas, S.; Lundin, R.: Upper ionosphere of Mars is not axially symmetrical. Earth, Planets and Space 64, pp. 113 - 120 (2012)
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).
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.
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.