Mierla, M.; Inhester, B.; Zhukov, A. N.; Shestov, S. V.; Bemporad, A.; Lamy, P.; Koutchmy, S.: Polarimetric Studies of a Fast Coronal Mass Ejection. Solar Physics 297, p. 78 (2022)
Ying, B.; Feng, L.; Inhester, B.; Mierla, M.; Gan, W.; Lu, L.; Li, S.: Three-dimensional analyses of an aspherical coronal mass ejection and its driven shock. Astronomy and Astrophysics 660, p. A23 (2022)
Inhester, B.; Mierla, M.; Shestov, S.; Zhukov, A.: Error Estimation of Linear Polarization Data from Coronagraphs – Application to STEREO-A/SECCHI-COR1 Observations. Solar Physics 296, 72 (2021)
Cheng , X.; Zhang, J.; Kliem, B.; Török, T.; Xing, C.; Zhou, Z. J.; Inhester, B.; Ding, M. D.: Initiation and Early Kinematic Evolution of Solar Eruptions. The Astrophysical Journal 894 (2), 85 (2020)
Dai, X.; Wang, H.; Inhester, B.: Electron Density Reconstruction of Solar Coronal Mass Ejections Based on a Genetic Algorithm: Method and Application. The Astrophysical Journal 896 (2), 155 (2020)
Feng, L.; Li, H.; Inhester, B.; Chen, B.; Ying, B.-L.; Lu, L.; Gan, W.: On the error analyses of polarization measurements of the white-light coronagraph aboard ASO-S. Research in Astronomy and Astrophysics 19 (4), 059 (2019)
Lu, L.; Inhester, B.; Feng, L.; Liu, S.; Zhao, X.: Measure the Propagation of a Halo CME and Its Driven Shock with the Observations from a Single Perspective at Earth. Astrophysical Journal 835 (2), 188 (2017)
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)
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).
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 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.