EGU23-11192, updated on 24 Oct 2023
https://doi.org/10.5194/egusphere-egu23-11192
EGU General Assembly 2023
© Author(s) 2023. This work is distributed under
the Creative Commons Attribution 4.0 License.

Ion reflection observed at high Mach number interplanetary shocks: Solar Orbiter observations

Andrew Dimmock1, Michael Gedalin2, Domenico Trotta3, Ahmad Lalti1, Daniel Graham1, Yuri Khotyaintsev1, Rami Vainio4, Xochitl Blanco-Cano5, Primoz Kajdič5, and Christopher Owen6
Andrew Dimmock et al.
  • 1Swedish Institute of Space Physics (IRF), Uppsala, Sweden (andrew.dimmock@irfu.se)
  • 2Department of Physics, Ben-Gurion University of the Negev, Beer-Sheva, Israel
  • 3Imperial College London, London, UK
  • 4University of Turku, Turku, Finland
  • 5Departamento de Ciencias Espaciales, Instituto de Geofísica, Universidad Nacional Autónoma de México, Ciudad Universitaria, Ciudad de México, Mexico
  • 6Mullard Space Science Laboratory, University College London, UK

Collisionless shocks exist across diverse plasma environments. Examples are supernova remnants, comets, near planets, and interplanetary (IP) shocks in the solar wind. As the shock Mach number increases, so does the complexity of the ion distribution functions at the shock front due to features such as whistler precursors, ion reflection, shock ripples, and nonstationarity. 

Experimental studies of ion dynamics at supercritical high Mach (>5) number shocks are typically conducted using planetary bow shock crossings since the Mach number of these shocks are higher while the shock speeds with respect to the observing spacecraft are lower. As a result, it is easier to resolve complex features in the ion velocity distribution function. For these reasons, studies concentrating on ion reflection at IP shocks are rare. However, comparisons with IP shocks are interesting since they have a much larger curvature radius and can be accompanied by more energetic particles.

In this work, we analyze a quasi-perpendicular shock observed by Solar Orbiter (SolO) on 30 October 2021 with a Mach number of around 7; this is much higher than the typical values of SolO IP shocks, which are between 1-3. For this event, we observed clear signatures in the upstream ion distribution function of reflected ions with energies extending to around 15 keV, which is lower than reported by other studies. The shock also demonstrates a non-planar feature, which may indicate shock rippling. In addition, whistler precursors are also found immediately upstream locally within the shock foot. We present these experimental results and a comparison with test-particle analysis and numerical modeling results.

How to cite: Dimmock, A., Gedalin, M., Trotta, D., Lalti, A., Graham, D., Khotyaintsev, Y., Vainio, R., Blanco-Cano, X., Kajdič, P., and Owen, C.: Ion reflection observed at high Mach number interplanetary shocks: Solar Orbiter observations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11192, https://doi.org/10.5194/egusphere-egu23-11192, 2023.