Fränz, M.; Dubinin, E.; Andrews, D.; Nilsson, H.; Barabash, S.; Fedorov, A.: Cold Ion Escape from the Martian Ionosphere. European Planetary Science Congress, Nantes, France (2015)
Barabash, S.; Holmsrtom, M.; Futaana, Y.; Fedorov, A.; Frahm, R.; Fraenz, M.; Dubinin, E.: Phobos-solar wind interaction: Results from Mars Express for the closest-ever fly-by. European Geosciences Union General Assembly 2014, Vienna, Austria (2014)
Dubinin, E.; Fraenz, M.; Mazelle, C.; Barabash, S.: Large-amplitude coherent structures in plasma near Mars. The 5th Moscow Solar System Symposium (5M-S3), Moscow, Russia (2014)
Dubinin, E.; Fraenz, M.; Zhang, T.-L.; Woch, J.; Wei, Y.: Ionospheric magnetic fields and currents at Venus and Mars. European Geosciences Union General Assembly 2014, Vienna, Austria (2014)
Dubinin, E.; Fraenz, M.; Zhang, T.-L.; Woch, J.; Wei, Y.: Ionospheric magnetic fields at Venus and Mars and their effect on plasma flow in the near planet wakes. EPSC, Estoril, Portugal (2014)
Dubinin, E.; Fraenz, M.; Zhang, T.-L.; Woch, J.; Wei, Y.; Barabash, S.: Asymmetrical response of the ionospheric magnetization and the plasma sheet formation on the IMF orientation. 6th Alfven Conference: Plasma Interactions with Solar System Objects anticipating Rosetta, MAVEN and Mars Orbiter Mission, London, UK (2014)
Wei, Y.; Fränz, M.; Dubinin, E.; Wan, W.; Jarvinen, R.; Zhang, T.-L.; Barabash, S.; Lundin, R.: Ablation of Venusian oxygen ions by unshocked solar wind. European Geosciences Union General Assembly 2014, Vienna, Austria (2014)
Fan, K.; Wei, Y.; Fränz, M.; Dubinin, E. M.; Mcfadden, J.: Efficiency of Solar wind electric field in accelerating planetary ions. EPSC-DPS Joint Meeting 2019, Geneva, Switzerland (2019)
Fränz, M.; Dubinin, E. M.; Fan, K.; Maes, L.; Halekas, J.; McFadden, J.; Connerney, J.: Mars in the Solar Wind - Simulations and Observations. EPSC-DPS Joint Meeting 2019, Geneva, Switzerland (2019)
Fränz, M.; Dubinin, E. M.; Fan, K.; Maes, L.; Halekas, J.; McFadden, J.: Mars in the Solar Wind. 21st EGU General Assembly, EGU2019, Vienna, Austria (2019)
Chai, L.; Wei, Y.; Wan, W.; Zhang, T.; Fraenz, M.; Dubinin, E.; Zhang, H.; Rong, Z.; Barabash, S.: An induced global magnetic field looping around the magnetotail of Venus. European Geosciences Union General Assembly, Vienna, Austria (2016)
Han, Q.; Wei, Y.; Chai, L.; Rong, Z.; Fraenz, M.; Dubinin, E.; Wan, W.; Rong, Z.; Futaana, Y.: EUV0dependence of Venusian ionopause height over the dayside high-latitude region: VEX and PVO observations. European Geosciences Union General Assembly, Vienna, Austria (2016)
Dubinin, E.; Fraenz, M.; Andrews, D.; Witasse, O.; Barabash, S.: Ionosphere of Mars as seen by Mars Express. Effect of crustal fields. European Planetary Science Congress, Nantes, France (2015)
Fränz, M.; Dubinin, E.; Andrews, D.; Nilsson, H.; Barabash, S.; Fedorov, A.: Cold Ion Escape from the Martian Ionosphere - 2007-2014. European Geosciences Union General Assembly, Vienna, Austria (2015)
Fraenz, M.; Dubinin, E.; Andrews, D.; Nilsson, H.; Fedorov, A.: Cold ion escape from the Martian ionosphere. European Geosciences Union General Assembly 2014, Vienna, Austria (2014)
Han, X.; Fraenz, M.; Andrews, D.; Dubinin, E.; Wan, W.; Barabash, S.: The control of Martian ionopause altitude by the crustal and induced magnetic field strength. European Geosciences Union General Assembly 2014, Vienna, Austria (2014)
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.