Telloni, D.; Antonucci, E.; Adhikari, L.; Zank, G. P.; Giordano, S.; Vai, M.; Zhao, L.-L.; Andretta, V.; Burtovoi, A.; Capuano, G. E.et al.; Da Deppo, V.; De Leo, Y.; Fineschi, S.; Grimani, C.; Heinzel, P.; Jerse, G.; Landini, F.; Liberatore, A.; Moses, J. D.; Naletto, G.; Nicolini, G.; Pancrazzi, M.; Romoli, M.; Russano, G.; Sasso, C.; Slemer, A.; Spadaro, D.; Stangalini, M.; Susino, R.; Teriaca, L.; Uslenghi, M.; Sorriso-Valvo, L.; Marino, R.; Perrone, D.; D'Amicis, R.; Bruno, R.: First polar observations of the fast solar wind with the Metis - Solar Orbiter coronagraph: Role of 2D turbulence energy dissipation in the wind acceleration. Astronomy and Astrophysics 670, p. L18 (2023)
Sasso, C.; Lagg, A.; Solanki, S. K.: Milne-Eddington inversions of the He I 10 830 Å{} Stokes profiles: influence of the Paschen-Back effect. Astronomy and Astrophysics 456, pp. 367 - 371 (2006)
Sasso, C.; Lagg, A.; Solanki, S. K.; Socas-Navarro, H.: Influence of the Paschen-Back effect on the results of polarimetric inversions of the He I 10830 Å triplet. Memorie della Societa Astronomica Italiana Supplement 9, p. 126 (2006)
Sasso, C.; Lagg, A.; Solanki, S. K.: Spectropolarimetry in the chromospheric He I 1083.0 nm multiplet. In: 1st Workshop of Astronomy and Astrophysics for Students, pp. 43 - 46 (Eds. Napolitano, N. R.; Paolillo, M.). INFN-Naples (2007)
Sasso, C.; Lagg, A.; Solanki, S. K.; Aznar Cuadrado, R.; Collados, M.: Full-Stokes Observations and Analysis of He I 10830 Å in a Flaring Region. In: The Physics of Chromospheric Plasmas, p. 467 (Eds. Heinzel, P.; I., D.; R. J., R.). (2007)
Sasso, C.; Lagg, A.; Solanki, S. K.; Aznar Cuadrado, R.; Collados, M.: Full-Stokes observations and analysis of He I 10830 Å in a flaring region. In: The Physics of Chromospheric Plasmas, pp. 467 - 471 (Eds. Heinzel, P.; Dorotovič, I.; Rutten, R. J.). ASP, San Francisco (2007)
Sasso, C.; Lagg, A.; Solanki, S. K.: Influence of the Paschen-Back effect on the Stokes profiles of the HE 10830 Å triplet. In: Proceedings of the International Scientific Conference on Chromospheric and Coronal Magnetic Fields (Eds. Innes, D. E.; Lagg, A.; Solanki, S. K.; Danesy, D.). ESA Publ. Div., Noordwijk (2005)
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.