Castellanos Durán, J. S.; Kleint, L.: The Statistical Relationship between White-light Emission and Photospheric Magnetic Field Changes in Flares. The Astrophysical Journal 904 (2), 96 (2020)
Castellanos Durán, J. S.; Kleint, L.; Calvo-Mozo, B.: A Statistical Study of Photospheric Magnetic Field Changes During 75 Solar Flares. The Astrophysical Journal 852 (1), 25 (2018)
Albert, K.; Hirzberger, J.; Busse, D.; Castellanos Durán, J. S.; Kolleck, M.: Metadata and Their Importance in SO/PHI's On–Board Data Processing. In: Astronomical Data Analysis Software and Systems XXIX (ASP Conference Series), Vol. 527, pp. 599 - 602 (Ed. Pizzo, R.). (2020)
Albert, K.; Hirzberger, J.; Busse, D.; Blanco Rodriguez, J.; Castellanos Durán, J. S.; Cobos Carrascosa, J. P.; Fiethe, B.; Gandorfer, A. M.; Guan, Y.; Kolleck, M.et al.; Lagg, A.; Lange, .; Michalik, H.; Solanki, S. K.; Iniesta, J. C. D. T.; Woch, J.: Performance Analysis of the SO/PHI Software Framework for On-board Data Reduction. In: Astronomical Data Analysis Software and Systems XXVIII, Vol. 523, pp. 151 - 154 (Eds. Teuben, P. J.; Pound, M. W.; Thomas, B. A.; Warner, E. M.). Astronomical Society of the Pacific, San Francisco (2019)
Sowmya, K.; Lagg, A.; Solanki, S. K.; Castellanos Durán, J. S.: Fast downflows in a chromospheric filament. In: Proceedings of the International Astronomical Union: Solar and Stellar Magnetic Fields: Origins and Manifestations, Vol. 15, pp. 454 - 457 (Ed. Kosovichev, A.). Symposium S354 (Solar and Stellar Magnetic Fields: Origins and Manifestations). (2019)
Albert, K.; Hirzberger, J.; Busse, D.; Rodrguez, J. B.; Castellanos Durán, J. S.; Carrascosa, J. P. C.; Fiethe, B.; Gandorfer, A. M.; Guan, Y.; Kolleck, M.et al.; Lange, T.; Michalik, H.; Solanki, S. K.; Iniesta, J. C. d. T.; Woch, J.: Performance analysis of the SO/PHI software framework for on-board data reduction. 28th annual international Astronomical Data Analysis Software & Systems (ADASS) conference, College Park, Maryland, USA (2019)
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.
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".