Feldman, U.; Dammasch, I. E.; Landi, E.; Doschek, G. A.: Observations indicating that ≈ 1 × 107 K solar flare plasmas may be produced in situ from ≈ 1 × 106 K coronal plasma. Astrophysical Journal 609, pp. 439 - 451 (2004)
Feldman, U.; Landi, E.; Doschek, G. A.; Dammasch, I. E.; Curdt, W.: Free-free emission in the far-ultraviolet spectral range: A resource for diagnosing solar and stellar flare plasmas. Astrophysical Journal 593, pp. 1226 - 1241 (2003)
Wilhelm, K.; Lemaire, P.; Dammasch, I. E.; Hollandt, J.; Schühle, U.; Curdt, W.; Kucera, T.; Hassler, D. M.; Huber, M. C. E.: Solar irradiances of ultraviolet emission lines measured during the minimum of sunspot activity in 1996 and 1997. Physics and Chemistry of the Earth C, 25, pp. 389 - 392 (2000)
Wilhelm, K.; Schühle, U.; Curdt, W.; Dammasch, I. E.; Hollandt, J.; Lemaire, P.; Huber, M. C. E.: Solar spectroradiometry with the telescope and spectrograph SUMER on the Solar and Heliospheric Observatory SOHO. Metrologia 37, pp. 393 - 398 (2000)
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).
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.
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 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.