Multispacecraft Study of the Interaction Between an Interplanetary Shock and a Solar Wind Flux Rope. Issue 12 (9th December 2019)

• Record Type: Journal Article
• Authors: Blanco‐Cano, X.; Burgess, D.; Sundberg, T.; Kajdič, P.
• Is Part Of: Journal of geophysical research. Volume 124:Issue 12(2019)
• Page Start: 9760
• Page End: 9773
• Publication Date: 2019-12-09
• Subjects: solar wind -- shocks -- flux ropes -- energetic solar particles -- foreshocks; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1029/2019JA026748
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract: Interplanetary (IP) shocks are driven in the heliosphere by fast coronal ejecta, they can accelerate particles and are associated with solar energetic particle and energetic storm particle events. IP shocks can interact with structures in the solar wind and with magnetospheres. We show how the properties of an IP shock change when it interacts with a small‐scale flux rope‐like structure (FRLS). Data from Cluster, Wind, and ACE show that the spacecraft observed the shock‐FRLS interaction at different stages of evolution. Wind and ACE observed the FRLS at shock crossing; Cluster observed the FRLS downstream, after it had crossed the shock. The shock‐FRLS interaction changes shock geometry, affecting ion injection processes, energetic particles fluxes, and the upstream/downstream regions. While Wind and ACE observed a quasi‐perpendicular shock, Cluster crossed a quasi‐parallel shock and a foreshock with a variety of ion distributions. The FRLS modified the shock on scales of at least ∼ 10–20 R E . The complexity of the ion foreshock measured by Cluster is explained by the dynamics of the shock transitioning from quasi‐perpendicular to quasi‐parallel and the geometry of the magnetic field within the flux rope. Fluxes of particles with energy up to 125 keV are affected by the FRLS‐shock interaction, modulating the associated energetic storm particle event. The interaction of a FRLS with an IP shock has not been discussed before using multispacecraft observations. Interactions like this should occur often along the shock fronts; hence, they are important for a better understanding of shock structure, evolution, and particle acceleration. Key Points: Shock interaction with small flux ropes in the solar wind can change shock geometry and impact ion injection at the shock Interplanetary shock interaction with flux ropes can modify the upstream and downstream regions Fluxes of particles with energy up to 125 keV are affected by the FRLS‐shock interaction, modulating associated ESP events