McKenzie, J. F.; Dubinin, E.; Sauer, K.: Nonlinear waves propagating transverse to the magnetic field. Journal of Plasma Physics 65, pp. 213 - 233 (2001)
McKenzie, J. F.; Sauer, K.; Dubinin, E.: Stationary waves in a bi-ion plasma transverse to the magnetic field. Journal of Plasma Physics 65, pp. 197 - 212 (2001)
Sauer, K.; Dubinin, E.; McKenzie, J. F.: New type of soliton in bi-ion plasmas and possible implications. Geophysical Research Letters 28, pp. 3589 - 3592 (2001)
Axford, W. I.; McKenzie, J. F.; Sukhorukova, G. V.; Banaszkiewicz, M.; Czechowski, A.; Ratkiewicz, R.: Acceleration of the high speed solar wind in coronal holes. Space Science Reviews 87, pp. 25 - 41 (1999)
McKenzie, J. F.; Sukhorukova, G. V.; Axford, W. I.: The temperature and density structure in the closed field regions of the solar corona. Astronomy and Astrophysics 350, pp. 1035 - 1039 (1999)
Shukla, P. K.; Bingham, R.; McKenzie, J. F.; Axford, W. I.: Solar coronal heating by high-frequency dispersive Alfvén waves. Solar Physics 186, pp. 61 - 66 (1999)
Woodward, T. I.; McKenzie, J. F.: Stationary incompressible MHD perturbations generated by a current source in a moving plasma. Planetary and Space Science 47, pp. 545 - 555 (1999)
Czechowski, A.; Ratkiewicz, R.; McKenzie, J. F.; Axford, W. I.: Heating and acceleration of minor ions in the solar wind. Astronomy and Astrophysics 335, pp. 303 - 308 (1998)
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.