Attie, R.; Innes, D. E.; Solanki, S. K.; Glassmeier, K.-H.: Relationship between supergranulation flows, magnetic cancellation and network flares. Astronomy and Astrophysics 596, A15 (2016)
Yousefzadeh, M.; Safari, H.; Attie, R.; Alipour, N.: Motion and Magnetic Flux Changes of Coronal Bright Points Relative to Supergranular Cell Boundaries. Solar Physics 291, pp. 29 - 39 (2015)
Attie, R.; Innes, D. E.; Potts, H. E.: Evidence of photospheric vortex flows at supergranular junctions observed by FG/SOT (Hinode). Astronomy and Astrophysics 493 (2), pp. L13 - L16 (2009)
Innes, D. E.; Genetelli, A.; Attie, R.; Potts, H. E.: Quiet Sun mini-coronal mass ejections activated by supergranular flows. Astronomy and Astrophysics 495, p. 319 (2009)
Innes, D. E.; Attie, R.; Hara, H.; Madjarska, M. S.: EIS/ Hinode Observations of Doppler Flow Seen through the 40-Arcsec Wide-Slit. Solar Physics 252, pp. 283 - 292 (2008)
Attie, R.; Innes, D. E.: Explosive Event in the Quiet Sun Seen by XRT-EIS and SUMER. In: First Results From Hinode, p. 155 (Eds. Matthews, S. A.; Davis, J. M.; Harra, L. K.). Astronomical Society of the Pacific, San Francisco (2008)
Attie, R.: The relationship between supergranulation flows, magnetic field evolution and network flares. Dissertation, Tech. Univ. Braunschweig, Braunschweig, Braunschweig (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.