Zeuner, F.; Feller, A.; Iglesias, F. A.; Solanki, S. K.: Detection of spatially structured scattering polarization of Sr I 4607.3 Å with the Fast Solar Polarimeter. Astronomy and Astrophysics 619, A179 (2018)
Iglesias, F. A.; Feller, A.; Nagaraju, K.; Solanki, S. K.: High-resolution, high-sensitivity, ground-based solar spectropolarimetry with a new fast imaging polarimeter. Astronomy and Astrophysics 590, A89 (2016)
Feller, A.; Iglesias, F. A.; Nagaraju, K.; Solanki, S. K.; Ihle, S.: Fast Solar Polarimeter: Description and First Results. In: Solar Polarization 7, Vol. 489, pp. 271 - 277 (Eds. Nagendra, K. N.; Stenflo, J. O.; Qu, Z. Q.; Sampoorna, M.). Astronomical Society of the Pacific, Utah, USA (2014)
van Noort, M.; Feller, A.; Iglesias, F. A.; Doerr, H.-P.: Image restoration with a grating spectro-polarimeter at the SST and plans for GREGOR/GRIS. 2nd GREGOR/SOLARNET science meeting, Göttingen, Germany (2016)
Iglesias, F. A.: Development of a high-cadence, high-precision solar imaging polarimeter with application to the FSP prototype. Dissertation, Techn. Univ. Carolo-Wilhelmina, Braunschweig, Braunschweig (2016)
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.
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.
How does our star heat its outer atmosphere, the solar corona, to unimaginable temperatures of up to 10 million degrees Celsius? With unprecedented observational data from ESA's Solar Orbiter spacecraft and powerful computer simulations, ERC starting grant awardee Pradeep Chitta intends to bring new momentum to the search for the coronal heating mechanism.
The research group “Solar Lower Atmosphere and Magnetism” (SLAM) studies the conditions and dynamic processes in the atmospheric layer between the solar surface (photosphere) and the overlying chromosphere, an approximately 2000 km thick gas layer.
The main research fields of the department "Sun and Heliosphere" are covered by the research groups "Solar and Stellar Coronae", "Solar Lower Atmosphere and Magnetism", "Solar and Stellar Magnetohydrodynamics" and "Solar Variability and Climate".