White, T. R.; Benomar, O.; Silva Aguirre, V.; Ball, W. H.; Bedding, T. R.; Chaplin, W. J.; Christensen-Dalsgaard, J.; Garcia, R. A.; Gizon, L.; Stello, D.et al.; Aigrain, S.; Antia, H. M.; Appourchaux, T.; Bazot, M.; Campante, T. L.; Creevey, O. L.; Davies, G. R.; Elsworth, Y. P.; Gaulme, P.; Handberg, R.; Hekker, S.; Houdek, G.; Howe, R.; Huber, D.; Karoff, C.; Marques, J. P.; Mathur, S.; McQuillan, A.; Metcalfe, T. S.; Mosser, B.; Nielsen, M. B.; Régulo, C.; Salabert, D.; Stahn, T.: Kepler observations of the asteroseismic binary HD 176465. Astronomy and Astrophysics 601, A82 (2017)
White, T. R.; Pope, B. J. S.; Antoci, V.; Papics, P. I.; Aerts, C.; Gies, D. R.; Gordon, K.; Huber, D.; Schaefer, G. H.; Aigrain, S.et al.; Albrecht, S.; Barclay, T.; Barentsen, G.; Beck, P. G.; Bedding, T. R.; Andersen, M. F.; Grundahl, F.; Howell, S. B.; Ireland, M. J.; Murphy, S. J.; Nielsen, M. B.; Aguirre, V. S.; Tuthill, P. G.: Beyond the Kepler/K2 bright limit: variability in the seven brightest members of the Pleiades. Mon. Not. Roy. Astron. Soc. 471 (3), pp. 2882 - 2901 (2017)
Garcia, R. A.; Ceillier, T.; Salabert, D.; Mathur, S.; van Saders, J. L.; Pinsonneault, M.; Ballot, J.; Beck, P. G.; Bloemen, S.; Campante, T. L.et al.; Davies, G. R.; do Nascimento Jr., J.-D.; Mathis, S.; Metcalfe, T. S.; Nielsen, M. B.; Suárez, J. C.; Chaplin, W. J.; Jiménez, A.; Karoff, C.: Rotation and magnetism of Kepler pulsating solar-like stars. Towards asteroseismically calibrated age-rotation relations. Astronomy and Astrophysics 572, A34 (2014)
Lund, M. N.; Lundkvist, M.; Silva Aguirre, V.; Houdek, G.; Casagrande, L.; Van Eylen, V.; Campante, T. L.; Karoff, C.; Kjeldsen, H.; Albrecht, S.et al.; Chaplin, W. J.; Nielsen, M. B.; Degroote, P.; Davies, G. R.; Handberg, R.: Asteroseismic inference on the spin-orbit misalignment and stellar parameters of HAT-P-7. Astronomy and Astrophysics 570, A54 (2014)
Nielsen, M. B.; Gizon, L.; Schunker, H.; Karoff, C.: Rotation periods of 12 000 main-sequence Kepler stars: Dependence on stellar spectral type and comparison with v sin i observations. Astronomy and Astrophysics 557, L10 (2013)
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.