Andretta, V.; Giampapa, M. S.; Covino, E.; Reiners, A.; Beeck, B.: Estimates of Active Region Area Coverage through Simultaneous Measurements of the He I λλ 5876 and 10830 Lines. Astrophysical Journal 839 (2), 97 (2017)
Cegla, H. M.; Lovis, C.; Bourrier, V.; Beeck, B.; Watson, C. A.; Pepe, F.: The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems. Astronomy and Astrophysics 588, A127 (2016)
Reiners, A.; Lemke, U.; Bauer, F.; Beeck, B.; Huke, P.: Radial velocity observations of the 2015 Mar. 20 eclipse A benchmark Rossiter-McLaughlin curve with zero free parameters. Astronomy and Astrophysics 595, A26 (2016)
Beeck, B.; Schüssler, M.; Cameron, R. H.; Reiners, A.: Three-dimensional simulations of near-surface convection in main-sequence stars - III. The structure of small-scale magnetic flux concentrations. Astronomy and Astrophysics 581, A42 (2015)
Beeck, B.; Schüssler, M.; Cameron, R. H.; Reiners, A.: Three-dimensional simulations of near-surface convection in main-sequence stars - IV. Effect of small-scale magnetic flux concentrations on centre-to-limb variation and spectral lines. Astronomy and Astrophysics 581, A43 (2015)
Beeck, B.; Cameron, R. H.; Reiners, A.; Schüssler, M.: Three-dimensional simulations of near-surface convection in main-sequence stars II. Properties of granulation and spectral lines. Astronomy and Astrophysics 558, A49 (2013)
Beeck, B.; Collet, R.; Steffen, M.; Asplund, M.; Cameron, R. H.; Freytag, B.; Hayek, W.; Ludwig, H.-G.; Schüssler, M.: Simulations of the solar near-surface layers with the CO5BOLD, MURaM, and Stagger codes. Astronomy and Astrophysics 539, A121 (2012)
Norris, C. M.; Beeck, B.; Unruh, Y.; Solanki, S.; Yeo, K. L.; Krivova, N.: Modelling the Spectral Contrasts of Stellar Faculae. In: The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (CS19), Uppsala, Sweden, 06-10 June 2016, Vol. CS19, 63 (Ed. Feiden, G. A.). (2016)
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, 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.
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.
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.