Bučík, R.; Innes, D. E.; Mall, U.; Korth, A.; Mason, G. M.; Gomez-Herrero, R.: Long-lasting 3He-rich solar energetic particle sources. STEREO SEP meeting, Laurel, Maryland, USA (2014)
Bickel, V. T.; Manconi, A.; Loew, S.; Mall, U.: Entering Schrödinger’s Pyroclastic Vent and PSR: A Trafficability Analysis for the next Generation of Lunar Exploration Rovers. EGU General Assembly 2019, Vienna, Austria (2019)
Mall, U.; Kloskowski, D.; Schmidt, H.; Bickel, V. T.; Basilevsky, A.; Bugiolacchi, R.: On the variability of lunar soil properties – bearing capacity. EGU General Assembly 2019, Vienna, Austria (2019)
Bickel, V. T.; Lanaras, C.; Manconi, A.; Loew, S.; Mall, U.: Automated Detection and Mapping of lunar Rockfalls using a CNN. 1st Swiss “Workshop on Machine Learning for Environmental and Geosciences” (MLEG2019), Dübendorf, Switzerland (2019)
Bickel, V. T.; Lanaras, C.; Manconi, A.; Loew, S.; Mall, U.: Automated detection of lunar rockfalls using a Convolutional Neural Network. AGU Fall Meeting, Washington, D.C., USA (2018)
Bickel, V. T.; Manconi, A.; Loew, S.; Mall, U.: Automatic Detection of Rockfalls with Deep Neural Networks: Lessons learned on the Moon and Mars. ESA Living Planet Symposium, Milan, Italy (2018)
Mall, U.; Schmidt , H.; Kloskowski, D.; Bickel, V. T.; Bugiolacchi, R.: Lunar Rock Boulders as a Tool in comparative Planetology to investigate Rock Weathering. 7th European Lunar Symposium , Manchester, U.K. (2018)
Boehnhardt, H.; Krueger, H.; Mall, U.: Assessing the Primordial Character of Comets and of 67P/Churyumov-Gerasimenko. 50th ESLAB Symposium 2016, Leiden, Netherlands (2016)
Jockers, K.; Boehnhardt, H.; Krueger, H.; Mall, U.: Assessing the Primordial Character of Comets and of 67P/Churyumov-Gerasimenko. COMETS 2016, Toulouse, France (2016)
First Light for Sunrise III: the first tests with real sunlight were successful. The balloon-borne solar observatory should be ready for launch at the end of May.
First icy cold, then midnight sun: at the Arctic Circle, the team will prepare the next flight of the balloon-borne solar observatory - and hopes for solar fireworks.
Astronomical teamwork: By combining data from Solar Orbiter and SDO, a group of researchers has unambiguously determined the magnetic field at the solar surface.
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.