- Laboratoire de Physique des Plasmas (LPP), CNRS, Observatoire de Paris, Sorbonne Université, Université Paris-Saclay, École polytechnique, Institut Polytechnique de Paris, 91120 Palaiseau, France (emanuele.cazzola@lpp.polytechnique.fr)
Interplanetary shocks (IPs) are ubiquitous in the Heliosphere, and are particularly relevant when associated to Stream Interaction Regions and Coronal Mass Ejections due to their great geomagnetic effectiveness on Earth. As their evolution and propagation may vary based on the different interplanetary conditions, it is crucial to study the shocks characteristics under different scenarios to gain a better understanding of the different types of interactions with the near-Earth environment.
In this work, we propose a systematic analysis of the evolution, propagation and characterization of self-consistently generated interplanetary shocks under different conditions, such as different interplanetary magnetic field intensity, direction and particles density, velocity, by means of hybrid computer simulations (fluid electrons, kinetic ions). The use of a hybrid formalism allows us to simulate large domains necessary for the shocks to form and evolve, by still retaining the kinetic information, which is fundamental to consider important kinetic effects, e.g., in supercritical shock-fronts.
In particular, upon setting up an initial steepening velocity profile between slower and faster velocities, we observe this profile to evolve in a two boundaries-structure, separated by a turbulent sheath. We first qualify these boundaries relative to the structure expected from steady shocks, we estimate their respective velocity and their compression factor. We also analyse the main characteristics of the turbulent sheath, which propages at an intermediate velocity with a enhanced magnetic field and transverse components in the magnetic field and velocity. All these features are consistent with observations of SIRs at 1 AU (e.g., Jian+, 2006). Moreover, we also discuss the effects of different IMF orientations on the shock dynamics, as the different kinetic effects between a quasi-perpendicular and quasi-parallel configuration at the shock can bring to significant differences in the shock-front propagation and the related donwstream sheath turbulence.
How to cite: Cazzola, E., Fontaine, D., and Savoini, P.: Self-consistently generated, evolving and propagating interplanetary shocks with 3D hybrid simulations, EGU General Assembly 2025, Vienna, Austria, 27 Apr–2 May 2025, EGU25-6853, https://doi.org/10.5194/egusphere-egu25-6853, 2025.
