Innes, D. E.; Bučík, R.; Guo, L.-J.; Nitta, N.: Observations of solar X-ray and EUV jets and their related phenomena. Astron. Nachrichten 337, pp. 1024 - 1032 (2016)
Innes, D. E.; Heinrich, P.; Inhester, B.; Guo, L.-J.: Analysis of UV and EUV emission from impacts on the Sun after 2011 June 7 eruptive flare. Astronomy and Astrophysics 592, A17 (2016)
Bučík, R.; Innes, D. E.; Guo, L.; Mason, G. M.; Wiedenbeck, M. E.: Observations of EUV waves in 3He-rich solar energetic particle events. Astrophysical Journal 812 (1), 53 (2015)
Innes, D.; Guo, L.; Huang, Y.-M.; Bhattacharjee, A.: IRIS Si IV Line Profiles: An Indication for the Plasmoid Instability During Small-scale Magnetic Reconnection on the Sun. Astrophysical Journal 813, pp. 86 - 96 (2015)
Guo, L.-J.; Huang, Y.-M.; Bhattacharjee, A.; Innes, D. E.: Rayleigh-Taylor Type Instabilities in the Reconnection Exhaust Jet as a Mechanism for Supra-Arcade Downflows in the Sun. Astrophysical Journal 796 (2), L29 (2014)
Innes, D. E.; Guo, L.-J.; Bhattacharjee, A.; Huang, Y.-M.; Schmit, D.: Observations of Supra-Arcade Fans: Instabilities at the Head of Reconnection Jets. Astrophysical Journal 796 (1), 27 (2014)
Bučík, R.; Innes, D. E.; Guo, L.; Mason, G. M.; Wiedenbeck, M. E.: Observations of a blast EUV wave in 3He-rich solar energetic particle sources. 14th Annual International Astrophysics Conference, Tampa, USA (2015)
Analyzing the high spatial resolution solar Ca II H and K emission data obtained by the SUNRISE mission and building a model of other stars more active than the Sun
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).
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.